Announcements
Please find here extended information and documents about GPI.
Citations
The primary references to be cited by users of GPI are:
- "First light of the Gemini Planet Imager", B. Macintosh et al. PNAS, 2014 "[PNAS]", "[arXiv]"
Design Reference Documents
The following two design documents contain a wealth of information on the instrument, its capabilities and modes.
- Operational Concepts Definition Document - Science overview, drivers and requirements, observing scenarios
- Functional & Performance Requirements Document - performance requirements at the top level and broken down by subsystem
GPI Data Reduction
Our team published a series of ten papers at the 2014 SPIE Astronomical Telescopes & Instrumentation meeting discussing in detail our understanding of GPI data and its analysis as of six months after first light. Readers are strongly encouraged to take a look!
- GPI Observational Calibrations I: Overview of the GPI data reduction pipeline. by Perrin et al.
- GPI Observational Calibrations II: Detector Performance and Characterization. by Ingraham et al.
- GPI Observational Calibrations III: Empirical Measurement Methods and Applications of High-Resolution Microlens PSFs. by Ingraham et al.
- GPI Observational Calibrations IV: Wavelength Calibration and Flexure Correction for the Integral Field Spectrograph. by Wolff et al.
- GPI Observational Calibrations V: Astrometry and Distortion. by Konopacky et al.
- GPI Observational Calibrations VI: Photometric and Spectroscopic Calibration for the Integral Field Spectrograph. by Maire et al.
- GPI Observational Calibrations VII: On-sky Polarimetric Performance of the Gemini Planet Imager. by Witorowicz et al.
- GPI Observational Calibrations VIII: Characterization and Role of the Satellite Spots. by Wang et al.
- GPI Observational Calibrations IX: Least Squares Inversion Flux Extraction. by Draper et al.
- GPI Observational Calibrations X: Non-Redundant Masking on GPI. by Greenbaum et al.
Below follows a list of recent papers showing the latest developments in GPI Pipeline and postprocessing developments:
GPI Instrument Reference
Polarimetry
Project Web Pages
- GPI Project Web Page - Main page for the GPI project, including links to technical publications
GPI Frequently Asked Questions
Q: Can I observe a target fainter than I magnitude 9 by using a nearby bright star as the AO star?
A: No, the basic principle with the GPI AO system is that the science target IS the AO star, thus the science field is centered on the guide star.
Q: Can I observe close similar magnitude binaries?
A: No, the AO system is designed such that any close similar magnitude binary would have a strong adverse impact on the AO performance, and possibly not even allow the closing of the AO loop.
Q: What is the airmass limit of the instrument as the OCDD (pg 39) says there's a 50-deg zenith limit?
A: The contrast curves should be generally good to about 30 degrees off zenith - there are no separate models for the 50 degree case. To first order, contrast would scale up as airmass ^12/5, but the performance is NOT guaranteed for Zenith distances larger than 50 degrees. Any proposal applying for Zenith distances larger than 50 degrees should take contact with the instrument scientist previous to submitting the proposal. The ADC is specified to work up to ZD=50 and thus both OIWFS performance is not guaranteed AND the centering of the science object on the coronographic mask will be adversely affected for large Zenith angles.
Q: What is the AO Guide Star magnitude limit of the instrument?
Q: Can I observe targets that are Imag > 9.0 in better-than-median seeing?
A: Testing has shown that with slower camera rates it will work at decreased performance at I=9+. However, it is unlikely that the performance would improve in IQ20 conditions, because GPI isn't designed to run slowly to take advantage of slow seeing. Further, performance at I=9+ would be very sensitive to the read noise on the wavefront sensor, and is thus a complex undertaking. One should always refer to the "Instrument Performance pages" for the latest updates to the limiting magnitudes.
Q: Do I need PSF stars for Polarization observations?
A: In the polarization mode you don't need to observe PSF reference stars, because the two orthogonal polarizations essentially serve as each other's PSFs, though one can contemplate using some other form of PSF subtraction if you want to obtain a total intensity image as a followup characterization observation.
Q: Can I do dithering?
A: The only dithering possible is going off to take sky frames (for K1 and K2 bands) in open loop. There is NO capability to dither on the detector with closed OIWFS loops.
Q:Can GPI keep the sky fixed on the detector?
A:NO, the masks in the instrument are fixed orientation and optimized with respect to a fixed Cassegrain angle. With the Cassegrain angle always fixed (and not adjustable) it means that the sky will always rotate around the detector optical axis determined by the OIWFS axis.
Q:Can I mix different observing modes in the same observation?
A:NO, each observing mode requires its own set of internal calibrations and thus each observing mode setup requires its own acquisition. Even a change of filter is its own observing mode so no mixing of filters in the same observation.
GPI Acronyms
ADC | Atmospheric Dispersion Corrector or Analog to Digital Converter (Depends on context) |
ADI | Angular Differential Imaging |
AEOS | Advanced Electro-Optical System (USAF Telescope on Maui) |
AGB | Asymptotic Giant Branch |
ALMA | Atacama Large Millimeter Array |
ATEUI | Acceptance Test and Engineering User Interface |
ALTAIR | ALTitude-conjugate Adaptive optics for the InfraRed |
AMNH | American Museum of Natural History |
AO | Adaptive Optics |
AOC | Adaptive Optics Computer |
API | Application Programming Interface |
APLC | Apodized Pupil Lyot Coronagraph |
AR | Anti Reflection (coating for tranmissive elements) |
AU | Astronomical Unit (1.495 X 1011 m) |
ATP | Acceptance and Test Plan |
AURA | Association of Universities for Research in Astronomy |
CAL | Calibration Subsystem |
CANOPUS | The optical bench and associated electronics. Everything that is within the box attached to the ISS. Other subsystems of GeMS include the BTO (Beam Transfer Optics), the laser and LSE (Laser Service Enclosure) and the LLT (Laser Launch Telescope). |
CCB | Change Control Board |
CCIT | Coherent Communications, Imaging and Targeting |
CCC | Closed Cycle Coolor (CCR) |
CCR | Closed Cycle Refrigerator (CCC) |
CDR | Critical Design Review |
CEH | Command Event Handler (GPI interface to GIAPI) |
CfAO | Center for Adaptive Optics |
CFHT | Canada France Hawaii Telescope |
CGS | Centimeter gram second system of units |
CoDR | Conceptual Design Review |
CoPI | Co-Principal Investigator |
CoPM | Co-Project Manager |
COR | Coronagraph |
CP | Cerro Pachon |
CVNDF | Continuously Variable Neutral Density Filter |
CWS | Cold Working Surface |
d | Subaperture size projected on the primary mirror (18 cm for GPI) |
D | Telescope primary mirror diameter (8.0 m for Gemini) |
DAC | Digital to Analog Convertor |
DAR | Differential Atmospheric Refraction |
DARPA | Defense Advanced Research Projects Agency |
DD | Double (image) difference |
DHS | Data Handling System |
DM | Deformable Mirror |
DMS | Document Management system |
DRP | Data Reduction Pipeline |
EFS | External Frame Structure |
EPICS | Experimental Physics and Industrial Control System |
ESO | European Southern Observatory |
ESO VLT | European Southern Observatory Very Large Telescope |
EXAOC | Extreme Adaptive Optics Coronagraph (original name for GPI) |
FDRP | Final Data Reduction Pipeline |
FEA | Finite Element Analysis |
FITS | Flexible Image Transport System |
FOV | Field Of View |
FPRD | Functional and Performance Requirements Document |
FPM | Focal Plane Mask |
FSM | Fine Steering Mirror |
FSS | Flexure Sensitive Structure |
FTR | Fourier Transform wavefront Reconstructor |
FWHM | Full Width at Half Maximum |
GCAL | Gemini Facility Calibration Unit |
GDSN | Gemini Data Storage network |
GeMS | Gemini MCAO System |
GLAO | Ground Layer Adaptive Optics |
GMOS | Gemini Multi Object Spectrograph |
GMP | Gemini Master Process |
GPI | Gemini Planet Imager |
GPOL | Gemini Polarization module (obsolete) |
GSAOI | Gemini South Adaptive Optics Imager |
HCIT | High Contrast Imaging Test bed |
HEBS | High Energy Beam Sensitive |
HIA | Herzberg Institute of Astrophysics |
HL | High Level |
ICD | Interface Control Document |
ICS | Instrument Control System |
IDL | Image Display Language (RSI Inc.) |
IFS | Integral Field Spectrograph |
IMF | Initial Mass Function |
INO | Institut Nationale d'Optique |
IR | Infrared-Red |
IRAS | Infra-Red Astronomy Satellite |
ISS | Instrument Support Structure |
IWD | Inner Working Distance |
JPL | Jet Propulsion Laboratory |
JWST | James Webb Space Telescope |
LAN | Local Area Network |
LAO | Laboratory for Adaptive Optics |
LLNL | Lawrence Livermore National Lab |
mas | milli-arcsec (4.848 nanoradian) |
M1 | Gemini primary mirror |
M2 | Gemini secondary mirror |
M3 | Gemini Tertiary (or science fold mirror) |
MCD | Motion Control Daemon |
MEMS | Micro Electro-Mechanical System |
MJ | Mass of Jupiter (1.8988 X 1027 kg) |
MK | Mauna Kea |
MWBS | Multi-Wavelength Beam Splitter |
MWI | Multi-Wavelength Imager |
N | Number of subapertures across the primary mirror (44 for GPI) |
NCP | Non-Common Path |
NDR | Non-Destructive Read |
NIRC2 | Near Infrared Camera 2 for adaptive optics at Keck |
NIRSPEC | Near Infrared Spectrometer instrument at Keck |
NRC | National Research Council (careful, there is an American and a Canadian one, separate entities) |
NSF | National Science Foundation |
NTP | Network Time Protocol |
OAP | Off Axis Parabola |
OCDD | Operational Concept Definition Document |
OCS | Observatory Control System |
ODRP | On-Line Data Reduction Pipeline |
OFC | Optimized-gain Fourier Control |
OIWFS | On-Instrument Wavefront Sensor |
OIWGS | On Instrument Wave Front Sensor |
OMSS | Opto-Mechanical Superstructure |
OSIRIS | OH-Suppressing Infrared Imaging Spectrograph at Keck |
OT | Observing Tool |
OWD | Outer Working Distance |
PA | Position Angle |
pc | Parsec (3.085 X 1016 m) |
PCS | Primary Control System |
PDR | Preliminary Design Review |
PE | Project Engineer |
PI | Principal Investigator |
Piezo | Piezo effect actuator |
PN | Planetary Nebula |
pnCCD | pnSensor based CCD. |
PM | Project Manager |
PPM | Pupil Plane Mask |
PS | Project Scientist |
PSDI | Phase-Shifting Diffraction Interferometer |
PSF | Point Spread Function |
PZT | Lead Zirconium Titanate (Piezo effect actuator) |
QE | Quantum Efficiency |
QPT | Queue Planning Tool |
RFP | Request for Proposal |
RMS | Root Mean Square |
ROC | Radius Of Curvature |
ROI | Region of Interest |
RPC | Remote Procedure Call |
RSS | Root Sum Square |
SC | Science Camera |
SCC | Supervisory and Component-Control Computer (Obsolete, see TLC) |
SCS | Gemini Telescope Secondary Control System |
SD | Simple (image) difference |
SE | Systems Engineer |
Seqexec | Sequence Executor |
SFWFS | Spatially Filtered Wave Front Sensor |
SNR | Signal to Noise Ratio |
SOW | Statement of Work |
SPIE | Society of Photoelectric Instrumentation Engineers |
SRD | Software Requirements Document |
SSDI | Simultaneous Spectral Differential Imaging |
SSD | Speckle Suppressing Device |
SSICD | Subsystem Interface Control Document |
SSRD | Subsystem Requirements Document |
STScI | Space Telescope Science Institute |
TBC | To Be Confirmed |
TBD | To Be Determined |
TCS | Telescope Control System |
TLC | Top Level Computer (for GPI was SCC) |
TMA | Three Mirror Anastigmat |
TPF | Terrestrial Planet Finder |
TRIDENT | Three Channel Differential Imager for CHF Telescope |
T/T | Tip/Tilt |
T/T/F | Tip/Tilt/Focus |
UCB | University of California, Berkeley |
UCLA | University of California, Los Angeles |
UCO | UCO/Lick Observatory |
UCSC | University of California, Santa Cruz |
UdeM | Université de Montréal |
USAF | United States Air Force |
VLT | Very Large Telescope |
WBS | Work Breakdown Structure |
WD | White Dwarf |
WFE | WaveFront Error |
WFS | WaveFront Sensor |
WIRCAM | Wide-Field Infrared Camera |
Historical
Everything below this point contain older information that isn't kept upto date.
-
Campaign Science: CfP and details
-
Early Science: CfP and details
-
GPIES Campaign: Details on the GPIES Campaign
-
Public Data from Commisioning observations
Accepted programs and status
GPI programs selected for Early Science Observations
The table below summarizes the programs that have been approved for GPI Early Science observations.
GPI ES Programs |
||||||
SV Program ID |
|
Title |
Band |
Time Awarded (hrs) |
Obs.Mode |
Status |
GS-2014A-SV-401 | A. Cheetham | Hidden under the coronagraph spot: transition disk exoplanets at 5AU scales |
|
|
Direct | Completed |
GS-2014A-SV-402 | L. Cieza | Observing planet formation in HD 135344B with GPI |
|
|
Coron-Pol, Coron | Completed |
GS-2014A-SV-403 | T. Currie | Directly Imaging Exoplanets Around Early-Type Stars in the Sco-Cen Association |
|
|
Coron | Completed |
GS-2014A-SV-404 | T. Davidge | Shedding Mass While Living Large: Circumsystem Disks Around Massive Algol BInaries |
|
|
Coron-Pol | Completed |
GS-2014A-SV-405 | M.Fitzgerald | High Fidelity Multiband Imaging Polarimetry of the Iconic Debris Disk System HR4796A |
|
|
Coron-Pol, Coron | Completed |
GS-2014A-SV-406 | J. Hashimoto | Exploring the HD 142527 disk at planet forming radii |
|
|
Coron-Pol | |
GS-2014A-SV-407 | M. Reggiani | Caught in the act: Confirming a young companion forming in the transitional disk around HD169142 |
|
|
Coron | Completed |
GS-2014A-SV-408 | R. Sahai | Caught in the Act: Imaging the central disk and outflow in V Hya, an AGB star in transition to a bipolar nebula |
|
|
Coron-Pol, Coron | Completed |
GS-2014A-SV-409 | G.S. Salter | Detection and Spectral Characterisation of a Doppler Companion |
|
|
Coron | Completed |
GS-2014A-SV-410 | P. Tuthill | The origin of Z CMa's enigmatic microjet |
|
|
Coron-Pol | Attempted |
GS-2014A-SV-411 | C. Melis | Probing the familiar but strange planetary systems around HD 131488 and HD 121191 |
|
|
Coron-Pol, Coron | Completed |
GS-2014A-SV-412 | J. Monnier | Imaging Planet Formation in situ with Gemini Planet Imager |
|
|
Coron-Pol | Completed |
GS-2014A-SV-413 | V. Rapson | Polarimetric Imaging of the Protoplanetary Disks TW Hya and V4046 Sgr |
|
|
Coron-Pol | Completed |
GS-2014A-SV-414 | T. Rodigas | The Circumbinary Environment of HD 142527 Revealed by GPI Polarized Differential Imaging |
|
|
Direct-Pol | Completed |
GS-2014A-SV-415 | P. Rojo | Investigating seasonal changes in Titan's meteorology through cloud monitoring with GPI |
|
|
Direct | Partially completed |
GS-2014A-SV-416 | T. Ueta | GPI-ES Investigations into the Circumstellar Shell Structure around the Bright Central Star of IRAS 11385-5517 |
|
|
Coron | Completed |
Call for Campaign Science Proposals
This page is also available as a pdf document.
The Gemini Observatory is pleased to announce a Call for Proposals for GPI Campaign Science. GPI is a technologically advanced instrument designed specifically for obtaining images and low-resolution spectra of faint objects and/or features very near to bright objects. While GPI’s primary science goal is the detection and characterization of exoplanets, its high contrast capabilities will allow significant scientific advances in the areas such as circumstellar disks, stellar evolution (mass transfer), fundamental stellar astrophysics (binaries) and solar system objects.
GPI is expected to be available for science use in Semester 2012B.
Proposals
GPI Campaign proposals should embrace a large, scientifically compelling, and statistically significant investigation in the chosen science area that cannot be achieved through the standard proposal mechanism. Gemini will choose the most scientifically compelling proposal or proposals for scheduling.
As GPI will require median or better observing conditions to operate effectively, all successful programs will be executed in queue mode. However, the Observatory encourages successful science teams to plan on spending significant time in Chile during the commissioning and early science period, so that they can gain a full understanding of GPI’s performance.
We will consider programs that request from 200 to 1000 queue hours of telescope time, spread over a maximum of six semesters. (The GSC has recommended that the total allocation for GPI Campaign Science programs not exceed 1400 hours; the Board will approve the final allocation following proposal review.) A maximum of 180 campaign hours per semester will be scheduled as science ranking band 1. Proposers may request time to be scheduled in band 2.
The standard proprietary period for data is 18 months after acquisition of individual observations. Proposals may request and justify a longer proprietary period for specific campaign observations.
Proposals should address any necessary precursor or followup observations needed to accomplish the science goals of the program and describe how these observations will be obtained. Allocation through the Campaign will be for use of GPI alone.
Collaboration of teams from across the Gemini partnership is encouraged, and partner participation is a criterion by which campaign proposals will be evaluated.
Proposals must include:
- a discussion of the primary scientific goals of the project;
- a description of the experimental design, including sample selection, use of GPI, scheduling requirements, calibration, etc.;
- a statement of the time requested by semester and by science ranking band;
- a description of data products compatible with the international virtual observatory to be delivered, and the timeline for their delivery;
- a management plan that describes staffing and resources available to complete the science program. The management plan must also describe
- the expected contributions of each participant;
- data management procedures, including access to data within the team;
- who is responsible for submitting progress reports and final reports;
- the process for redirecting the research agenda as discoveries are made;
- the mechanism for routine communication among research team members.
The scientific justification of the proposal, including relevant figures and captions, is limited to 5 pages. The experimental design, including figures and captions, is limited to 6 pages. The required management plan is limited to 3 pages. There is no page limit on references or target lists.
Proposals should be submitted via email to Gemini Deputy Director/Head of Science, Nancy Levenson, nlevenson at gemini.edu by 5:00PM HST on March 31, 2011 (03:00 GMT on April 1, 2011).
The Instrument
Details about the instrument and its expected performance are available in a separate document , and on the Gemini website. Please see the instruments section of the Gemini website, and current updates on GPI can be found at the external instrument site. Successful campaign proposers will be allowed to request minor adjustments to target lists and exposure times in light of actual on-sky performance of GPI. Gemini will be responsible for evaluating and approving these changes.
Research Collaboration Agreement
Each successful GPI Campaign Project will require a “Research Collaboration Agreement” signed by all members of the team before the campaign starts and submitted to the Gemini Deputy Director/Head of Science. The requirements of this agreement are described in the separate document: Policies for GPI Campaign Projects. The agreement should not be submitted with campaign proposals.
Program Review
Each successful GPI Campaign Project is to submit annual progress reports to the Gemini Director. These reports should contain (at a minimum) a summary of the observing time used thus far, comments on the quality of the data and whether the data quality is sufficient to meet the scientific goals of the program, a summary of the activities of each team member, the status of reduction of the data, and detailed plans for the next year of the project. The report should also indicate any preliminary science results arising from the project. Gemini and the GSC will assess these reports to determine if continuing campaign observations are warranted.
Early Science (SV) Call for Proposals
The Gemini Planet Imager (GPI) commissioning activities started in November 2013 and continue during the first semester of 2014. The commissioning is expected to be completed during the 2014B semester. Therefore, we invite the Gemini community to propose Early Science (ES) programs for GPI. Approximately six nights are available in April during the 2014A semester for this ES call.
Proposal submissions are due FRIDAY, FEBRUARY 28th, 2014, 23:59 UT .
The Early Science is way for the Gemini Community to get an early access to the instrument before it is offered in the 2014B semester. It is intended to be "end-to-end" testing, verifying the readiness of the entire system from observation preparation to data reduction. (The current version of the GPI IDL pipeline and data reduction package is now available from the instrument build team.) ES is also intended to exercise the instrument with a variety of observing programs and demonstrate to the community, through interesting and challenging science programs, the unique capabilities of GPI on Gemini South.
Commissioning is not yet complete, so performance information is preliminary and may not represent the final capability of GPI. All ES programs are undertaken in shared-risk mode. Updates will be provided as available on the GPI Status and Availability page, and notifications will be sent to the gpinews@gemini.edu mailing list, which is open to new subscribers.
Early Science proposals will be evaluated by the Gemini GPI Science Team including members from the Gemini Science and Technology Advisory Committee. Recommended programs will be forwarded to the Gemini Director for approval. Selection of ES programs will be done to ensure a wide range of types of target and observing modes. The different types of targets and approximate allocation times are given below. The allocated hours are notional only and will vary based on the programs selected. The proposed target observations must use the GPI Observing modes currently offered.
Available Observing Modes and approximate allocation times | |
Observing Mode | Allocated science time |
Coronography Y, J, H, K1 and K2 (IQ70CC50) | 10 hours |
Polarization Y, J, H, K1 and K2 (IQ70CC50) | 10 hours |
Direct Imaging or Polarization of Extended sources (i.e. any non-point source) (IQ70CC50) | 5 hours |
Direct Imaging or Polarization with no accurate photometry needed (IQ85CC70) | 10 hours |
Non-sidereal(1) | < 5 hours |
(1) Observations of non-sidereal targets have been very limited to-date, so success of programs in this mode is uncertain.
The approved Early Science Principal Investigators will be responsible for providing written, in-depth assessments of ES observations within two months of data acquisition. The data obtained during ES will be made available to the international Gemini community after a two-month proprietary period, and information from the assessments of the ES teams will be published on the Gemini web pages. PIs of approved programs are strongly encouraged to provide manuscripts of results to Gemini in advance of publication, especially to allow staff to review technical performance of the instrument. Community participation will help to ensure that GPI is a success when the system is in regular use.
GPI is an extreme adaptive-optics imaging polarimeter/integral-field spectrometer, which will provide diffraction-limited data between 0.9 and 2.4 microns. The system will provide contrast ratios of 10^6 on companions at separations of 0.2-1 arcsecond in a 1-2 hour observation. The science instrument will provide spectroscopy or dual-beam polarimetry of any object in the field of view. Bright natural guide stars (I<9 mag) are required for optimal performance of the GPI adaptive optics system. GPI will be capable of detecting point sources down to H = 23 mag., with ≥ 5-sigma, in 1 hour (absent photon noise from a bright companion). For more information on achievable contrast, see the Contrast Page.
CONSTRAINTS
1. Target visibility: We expect to observe ES programs between April 20, 2014 and April 26, 2014. Therefore the targets should have RAs between 08 hours and 19 hours and Declinations between +10 degrees and -70 degrees (elevation > 45 degrees). Note that GPI OIWFS reaches its specifications for Zenith angles <30 degrees and it will work down to <50 degrees but with limited performance.
2. OIWFS Guide stars: GPI uses the science target for its AO correction and thus the science target must have a V magnitude brighter than 9 and not be extended objects to achieve the full expected Strehl.
3. Observing conditions constraints: The following constraints are allowed:
- Image Quality(2): 70%-ile or 85%-ile.
- Sky Transparency (cloud cover): photometric (50%-ile).
- Sky Background: Any.
- Sky Transparency (Water vapor content): Any.
(2) Reasonable corrections are possible under poorer image quality conditions (up to 1" natural seeing or IQ=85%-ile). Proposers that do not require high Strehl limited images are encouraged to submit targets for these conditions. Details about the contrast and Strehl ratios that could be achieved with GPI for different seeing conditions can be found in the GPI Strehl web page.
4. Target Duplication: The GPI Science Campaign target list is available here and any target duplication between the Campaign and any proposed target is subject to the Target Duplication Policy for GPI, which is available here.
GUIDELINES
To submit a program, use the 2014A Phase I tool and include observing constraints, target lists, and GPI Meta Mode configuration information. Be sure to select "Other Proposal Types" and "System Verification" in the Proposal Class and the Proposal Type fields respectively, inside the Scheduling and Time Request section of the Phase I Tool.
The overheads associated with a GPI science observation can be estimated using the information given in the Sensitivity and Overheads web page. Science time requests should include these overheads.
PHASE I ADDITIONAL REQUIREMENTS
Scientific justification must be less than 1000 words. The technical justification should be sufficiently complete within its 1000 word limit that program feasibility can be assessed easily. A statement of data reduction plans must also be included in the technical justification. Proposers may use other data reduction tools in addition to the GPI IDL package. Selection for ES is based in part on the ability of the proposers to reduce the data and return feedback within a reasonable time.
By submitting an ES program the proposers agree to the following:
- There is no guarantee that the program will be observed.
- The proprietary period for ES data is two months.
- The PI will provide reduced data to Gemini for public release within two months of the completion ES program.
The GPI astronomers will assist PIs of the successfully accepted programs to complete the Phase II.
TIMELINE
February 5th | Call for ES proposals |
February 28th | Phase I deadline |
March 18th | Announcement of selected programs |
April 7th | Phase II deadline |
April 20th | Start of Early Science run |
Please, feel free to contact us with questions.
Sincerely,
The GPI team
Contacts: Fredrik T Rantakyro (frantaky@gemini.edu) and Pascale Hibon (phibon@gemini.edu).
Campaign Science
The first call to submit Campaign science proposals is available here, with a deadline of March 31, 2011.
The first call for letters of intent to submit Campaign science proposals was closed January 20, 2011. The call can be found here.
Early Science
The call for Early Science for GPI starts on February 5th, 2014. In this call the Gemini community is invited to propose Early science (ES) programs for GPI. The deadline for proposal submissions is February 28th, 2014. Approximately 6 nights of ES time is available in the 2014A semester. It is expected that the ES run will take place middle of April 2014 for 6 nights.
If you use any of these data in a publication, please include the standard Gemini acknowledgment:
Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil) and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina).
Early Science Target List
Early Science targets are listed below. Target duplication policies are described here.
ZCMa | 07:03:43.164 | -11:33:06.221 | Y, J, H Coron-Pol | |
VHya | 10:51:37.257 | -21:15:00.324 | H Coron, Y Coron-Pol | |
TWHya | 11:01:51.907 | -34:42:17.032 | J Coron, K2 Coron-Pol | |
IRAS11385-5517 | 11:40:58.806 | -55:34:25.817 | J Coron | |
BYCru | 12:04:48.785 | -62:00:08.582 | K2 Coron-Pol | |
WCru | 12:11:59.163 | -58:47:00.743 | K2 Coron-Pol | |
HD107649 | 12:22:24.855 | -51:01:34.349 | H Coron | |
HR4796A | 12:36:01.034 | -39:52:10.211 | J Coron, J, K1 Coron-Pol | |
HD110506 | 12:43:09.179 | -56:10:34.411 | H Coron | |
HD115600 | 13:19:19.540 | -59:28:20.437 | H Coron | |
HD118379 | 13:37:17.780 | -40:53:52.352 | H Coron | |
HD121191 | 13:55:18.859 | -53:31:43.028 | H Coron, H Coron-Pol | |
HD131488 | 14:55:08.026 | -41:07:13.421 | H Coron, H Coron-Pol | |
HD134331 | 15:10:41.610 | -43:43:47.533 | H Coron | |
HD135344B | 15:15:48.439 | -37:09:16.026 | J direct, J Coron, Y Coron-Pol | |
Titan | 15:25:19.300 | -16:15:34.100 | H, K1 Direct | |
HD142527 | 15:56:41.890 | -42:19:23.275 | Y,H Direct-Pol, H Coron-Pol | |
HD146606 | 16:18:16.160 | -28:02:30.154 | H Coron | |
MWC863 | 16:40:17.923 | -23:53:45.179 | J Coron-Pol | |
HD161743 | 17:48:57.926 | -38:07:07.478 | Y Direct-Pol | |
MWC275 | 17:56:21.288 | -21:57:21.870 | J Coron-Pol | |
V4046Sgr | 18:14:10.466 | -32:47:34.496 | J Coron, K2 Coron-Pol | |
HD169142 | 18:24:29.779 | -29:46:49.371 | J Direct, J Coron, J Coron-Pol |
GPI Campaign Target List
The GPI Campaign conducted a comprehensive survey to yield a robust census of extrasolar giant planets, and the Campaign concluded in semester 2018B. The campaign targets are listed below for historical reference.
Target duplication policies are described here.
HIP 159 | 00:02:02.6 | -02:45:58.2 | H-coron (~1 hr) | |||||||
HD 105 | 00:05:52.5 | -41:45:11.0 | H-coron (~1 hr) | |||||||
HR 9 | 00:06:50.1 | -23:06:27.1 | H-coron (~1 hr); H-coron-pol | |||||||
HD 377 | 00:08:26 | 06:37:00 | H-coron-pol; H-coron-pol | |||||||
HIP 795 | 00:09:51.6 | 08:27:11.5 | H-coron (~1 hr) | |||||||
HD 987 | 00:13:52.8 | -74:41:17.5 | H-coron (~1 hr) | |||||||
HD 984 | 00:14:10.2 | -07:11:56.8 | H-coron (~1 hr) | |||||||
HD 1237 | 00:16:12.7 | -79:51:04.0 | H-coron (~1 hr) | |||||||
HIP 1427 | 00:17:50.0 | 16:19:51.6 | H-coron (~1 hr) | |||||||
HD 1466 | 00:18:26.1 | -63:28:39.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 1803 | 00:22:51.8 | -12:12:34.0 | H-coron (~1 hr) | |||||||
HIP 2072 | 00:26:12.1 | -43:40:47.7 | H-coron (~1 hr) | |||||||
HIP 2472 | 00:31:25.0 | -48:48:12.7 | H-coron (~1 hr); H-coron-pol | |||||||
* bet01 Tuc | 00:31:32.6 | -62:57:29.5 | H-coron (~1 hr) | |||||||
HIP 2729 | 00:34:51.2 | -61:54:58.0 | H-coron (~1 hr) | |||||||
HIP 2841 | 00:36:00.8 | -59:43:01.9 | H-coron (~1 hr) | |||||||
HIP 3203 | 00:40:47.5 | -07:13:56.6 | H-coron (~1 hr) | |||||||
HIP 3210 | 00:40:51.6 | -53:12:35.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 3277 | 00:41:46.3 | -56:30:05.2 | H-coron (~1 hr) | |||||||
HIP 3540 | 00:45:11.0 | 00:15:11.8 | H-coron (~1 hr) | |||||||
HD 4944 | 00:50:24.3 | -64:04:04.0 | H-coron (~1 hr) | |||||||
HIP 4290 | 00:54:59.3 | 24:06:01.0 | H-coron (~1 hr) | |||||||
HIP 5373 | 01:08:45.7 | -25:51:40.0 | H-coron (~1 hr) | |||||||
HD 7112 | 01:09:56.6 | -64:21:33.1 | H-coron (~1 hr); H-coron-pol | |||||||
TYC 6427-030 | 01:12:40.5 | -29:10:46.5 | H-coron (~1 hr) | |||||||
HIP 5743 | 01:13:45.3 | 07:34:41.8 | H-coron (~1 hr) | |||||||
HD 8077 | 01:19:05.6 | -53:51:01.9 | H-coron (~1 hr) | |||||||
HIP 6276 | 01:20:32.3 | -11:28:03.7 | H-coron (~1 hr) | |||||||
HIP 6485 | 01:23:21.1 | -57:28:50.5 | H-coron (~1 hr) | |||||||
HIP 6494 | 01:23:25.6 | -76:36:42.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 6856 | 01:28:08.7 | -52:38:19.1 | H-coron (~1 hr) | |||||||
HIP 6960 | 01:29:36.1 | -21:37:45.5 | H-coron (~1 hr) | |||||||
HIP 7345 | 01:34:37.7 | -15:40:34.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 7576 | 01:37:35.4 | -06:45:36.7 | H-coron (~1 hr) | |||||||
HD 10800 | 01:37:55.6 | -82:58:30.0 | H-coron (~1 hr) | |||||||
HD 10472 | 01:40:24.1 | -60:59:56.6 | H-coron (~1 hr); H-coron-pol | |||||||
HD 10647 | 01:42:29.3 | -53:44:27.0 | H-coron (~1 hr); H-coron-pol | |||||||
tau Cet | 01:44:04 | -15:56:14 | H-coron-pol | |||||||
HIP 8241 | 01:46:06.3 | -53:31:19.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 8661 | 01:51:36.3 | -02:38:16.0 | H-coron (~1 hr) | |||||||
HD 12039 | 01:57:48.9 | -21:54:05.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 9892 | 02:07:18.0 | -53:11:56.4 | H-coron (~1 hr); H-coron-pol | |||||||
HD 13246 | 02:07:26.0 | -59:40:45.8 | H-coron (~1 hr); H-coron-pol | |||||||
HD 14228 | 02:16:30.6 | -51:30:44.0 | H-coron (~1 hr) | |||||||
HIP 10786 | 02:18:53.2 | -69:53:12.0 | H-coron (~1 hr) | |||||||
LP 353-51 | 02:23:26.6 | 22:44:06.7 | H-coron (~1 hr) | |||||||
HD 15279 | 02:25:52.0 | -52:57:52.1 | H-coron (~1 hr); H-coron-pol | |||||||
HD 15115 | 02:26:16.2 | 06:17:33.6 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 11964 | 02:34:22.6 | -43:47:47.0 | H-coron (~1 hr) | |||||||
HD 16699A | 02:38:44.2 | -52:57:03.0 | H-coron (~1 hr) | |||||||
TYC 8484-150 | 02:38:45.0 | -52:57:08.0 | H-coron (~1 hr) | |||||||
HD 16743 | 02:39:07.6 | -52:56:05.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 12394 | 02:39:35.2 | -68:16:00.8 | H-coron (~1 hr) | |||||||
HIP 12413 | 02:39:47.9 | -42:53:29.8 | H-coron (~1 hr) | |||||||
HIP 12444 | 02:40:12.4 | -09:27:10.4 | H-coron (~1 hr) | |||||||
zet Hor | 02:40:39.6 | -54:33:00.0 | H-coron (~1 hr) | |||||||
* 84 Cet B | 02:41:13.7 | -00:41:41.9 | H-coron (~1 hr) | |||||||
BD+05 378 | 02:41:25.8 | 05:59:18.4 | H-coron (~1 hr) | |||||||
HD 17051 | 02:42:33.5 | -50:48:01.1 | H-coron (~1 hr) | |||||||
HIP 12787 | 02:44:21.3 | 10:57:41.2 | H-coron (~1 hr) | |||||||
HIP 12837 | 02:45:01.1 | -22:09:58.7 | H-coron (~1 hr) | |||||||
HD 17390 | 02:46:45.1 | -21:38:22.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 13027B | 02:47:27.2 | 19:22:21.2 | H-coron (~1 hr) | |||||||
HD 17848 | 02:49:01.4 | -62:48:23.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 13359 | 02:51:53.0 | -61:37:05.0 | H-coron (~1 hr) | |||||||
HR 857 | 02:52:32.1 | -12:46:10.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 13847 | 02:58:15.7 | -40:18:17.0 | H-coron (~1 hr) | |||||||
HIP 14007 | 03:00:19.7 | -37:27:16.0 | H-coron (~1 hr) | |||||||
HIP 14551 | 03:07:50.8 | -27:49:52.0 | H-coron (~1 hr) | |||||||
LTT 1479 | 03:07:55.7 | -28:13:10.9 | H-coron (~1 hr) | |||||||
V* AE For | 03:08:06.6 | -24:45:34.7 | H-coron (~1 hr) | |||||||
IS Eri | 03:09:42.3 | -09:34:46.5 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 14857 | 03:11:52.5 | -39:01:23.2 | H-coron (~1 hr) | |||||||
HIP 15039 | 03:13:50.2 | -38:48:33.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 15353 | 03:17:59.1 | -66:55:36.6 | H-coron (~1 hr) | |||||||
HD 20631 | 03:18:41.1 | -18:33:34.6 | H-coron (~1 hr) | |||||||
HIP 15457 | 03:19:21.7 | 03:22:12.7 | H-coron (~1 hr) | |||||||
HD 21997 | 03:31:53.6 | -25:36:50.9 | H-coron (~1 hr); H-coron-pol | |||||||
eps Eri | 03:32:55.8 | -09:27:29.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 16846 | 03:36:47.3 | 00:35:15.9 | H-coron (~1 hr) | |||||||
HIP 17157 | 03:40:29.4 | -47:55:31.0 | H-coron (~1 hr) | |||||||
HIP 17338 | 03:42:39.8 | -20:32:43.8 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 17395 | 03:43:33.8 | -10:29:08.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 17695 | 03:47:23.3 | -01:58:19.9 | H-coron (~1 hr) | |||||||
HIP 17764 | 03:48:11.3 | -74:41:39.1 | H-coron (~1 hr); H-coron-pol | |||||||
HD 24071 | 03:48:35.4 | -37:37:19.2 | H-coron (~1 hr) | |||||||
HR 1190 | 03:48:35.8 | -37:37:12.5 | H-coron (~1 hr) | |||||||
HD 24224 | 03:48:47.3 | -53:10:56.2 | H-coron (~1 hr) | |||||||
HIP 18512 | 03:57:28.7 | -01:09:34.1 | H-coron (~1 hr) | |||||||
HIP 18714 | 04:00:31.9 | -41:44:54.2 | H-coron (~1 hr) | |||||||
HD 25457 | 04:02:36.7 | -00:16:08.1 | H-coron (~1 hr) | |||||||
HD 25570 | 04:03:56.6 | 08:11:50.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 22295 | 04:04:48:05. | -80:46:45.5 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 19076 | 04:05:20.3 | 22:00:32.0 | H-coron (~1 hr) | |||||||
HIP 19183 | 04:06:41.5 | 01:41:02.9 | H-coron (~1 hr) | |||||||
HD 26980 | 04:14:22.5 | -38:19:01.5 | H-coron (~1 hr) | |||||||
HIP 19855 | 04:15:25.8 | 06:11:58.7 | H-coron (~1 hr) | |||||||
HD 26923 | 04:15:28.8 | 06:11:12.7 | H-coron (~1 hr) | |||||||
gam Dor | 04:16:01.6 | -51:29:11.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 19990 | 04:17:15.7 | 20:34:43.5 | H-coron (~1 hr) | |||||||
HIP 20737 | 04:26:38.6 | -28:57:06.5 | H-coron (~1 hr); H-coron-pol | |||||||
51 Eri | 04:37:36.1 | -02:28:24.8 | H-coron (~4 hr); Y-coron (~4 hr); J-coron (~4 hr); K1-coron (~4 hr); K2-coron (~6 hr); J-POL (~4 hr) |
|||||||
HIP 21632 | 04:38:43.9 | -27:02:01.7 | H-coron (~1 hr) | |||||||
HD 29697 | 04:41:18.8 | 20:54:05.4 | H-coron (~1 hr) | |||||||
HIP 21965 | 04:43:17.2 | -23:37:41.9 | H-coron (~1 hr) | |||||||
HIP 22192 | 04:46:25.7 | -28:05:15.0 | H-coron (~1 hr); H-coron-pol | |||||||
HD 30447 | 04:46:49.5 | -26:18:09.0 | H-coron (~1 hr); H-coron-pol | |||||||
IX Eri | 04:47:36.3 | -16:56:04.0 | H-coron (~1 hr) | |||||||
HIP 22506 | 04:50:35.4 | -41:02:51.4 | H-coron (~1 hr) | |||||||
LP 776-25 | 04:52:24.4 | -16:49:21.9 | H-coron (~1 hr) | |||||||
HIP 22738 | 04:53:31.2 | -55:51:37.1 | H-coron (~1 hr) | |||||||
HD 31392 | 04:54:04.2 | -35:24:16.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 22844 | 04:54:53.0 | -58:32:51.5 | H-coron (~1 hr) | |||||||
HIP 22845 | 04:54:53.7 | 10:09:04.0 | H-coron (~1 hr); H-coron-pol | |||||||
CD-57 1054 | 05:00:47.1 | -57:15:25.4 | H-coron (~1 hr) | |||||||
HD 32372 | 05:00:51.8 | -41:01:06.7 | H-coron (~1 hr); H-coron-pol | |||||||
HD 32309 | 05:01:25.6 | -20:03:06.9 | H-coron (~1 hr) | |||||||
HD 32297 | 05:02:27.4 | 07:27:39.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 23554 | 05:03:53.3 | -24:23:17.0 | H-coron (~1 hr) | |||||||
zet Dor | 05:05:30.7 | -57:28:22.7 | H-coron (~1 hr) | |||||||
BD-21 1074 | 05:06:49.9 | -21:35:09.2 | H-coron (~1 hr) | |||||||
HIP 24362 | 05:13:37.3 | -32:04:01.8 | H-coron (~1 hr) | |||||||
HIP 24947 | 05:20:38.0 | -39:45:18.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 25127 | 05:22:42.7 | 13:13:45.1 | H-coron (~1 hr) | |||||||
* 111 Tau | 05:24:25.4 | 17:23:00.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 25283 | 05:24:30.1 | -38:58:10.2 | H-coron (~1 hr) | |||||||
CD-43 1846 | 05:26:22.9 | -43:22:36.4 | H-coron (~1 hr); H-coron-pol | |||||||
HD 35996 | 05:26:24.0 | -43:22:32.7 | H-coron (~1 hr); H-coron-pol | |||||||
HD 35841 | 05:26:36.6 | -22:29:23.7 | H-coron (~1 hr); H-coron-pol | |||||||
AF Lep | 05:27:04.8 | -11:54:03.5 | H-coron (~1 hr) | |||||||
HIP 25544 | 05:27:39.4 | -60:24:57.6 | H-coron (~1 hr) | |||||||
HIP 25627 | 05:28:28.0 | -39:22:15.6 | H-coron (~1 hr) | |||||||
HIP 25709 | 05:29:24.1 | -34:30:56.0 | H-coron (~1 hr) | |||||||
HIP 25746 | 05:29:50.1 | -47:04:34.7 | H-coron (~1 hr) | |||||||
TYC 5916-079 | 05:34:09.2 | -15:17:03.2 | H-coron (~1 hr) | |||||||
2MASS J0536 | 05:36:55.0 | -47:57:47.9 | H-coron (~1 hr) | |||||||
HIP 26395 | 05:37:08.8 | -11:46:31.7 | H-coron (~1 hr); H-coron-pol | |||||||
TYC 7604-167 | 05:37:13.2 | -42:42:57.3 | H-coron (~1 hr) | |||||||
HIP 26412 | 05:37:16.5 | -27:52:16.3 | H-coron (~1 hr) | |||||||
HD 37484 | 05:37:39.6 | -28:37:34.7 | H-coron (~1 hr); H-coron-pol | |||||||
HD 37478 | 05:39:17.1 | 10:15:35.4 | H-coron (~1 hr) | |||||||
HIP 26990 | 05:43:35.8 | -39:55:25.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 27134 | 05:45:13.4 | -59:55:26.0 | H-coron (~1 hr) | |||||||
HIP 27288 | 05:46:57.3 | -14:49:19.0 | H-coron (~1 hr); H-coron-pol | |||||||
beta Pic | 05:47:17.1 | -51:04:00.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 27371 | 05:47:49.5 | -40:03:50.0 | H-coron (~1 hr) | |||||||
HIP 27441 | 05:48:36.8 | -39:55:55.0 | H-coron (~1 hr) | |||||||
HD 40781 | 05:59:13.3 | -38:42:38.0 | H-coron (~1 hr) | |||||||
HIP 28498 | 06:00:55.3 | -54:57:05.0 | H-coron (~1 hr) | |||||||
HIP 28869 | 06:05:42.1 | -61:44:55.0 | H-coron (~1 hr) | |||||||
HIP 28921 | 06:06:16.6 | -27:54:21.2 | H-coron (~1 hr) | |||||||
CD-35 2722 | 06:09:19.2 | -35:49:31.1 | H-coron (~1 hr) | |||||||
V352 CMa | 06:13:45.3 | -23:51:43.0 | H-coron (~1 hr) | |||||||
HIP 29711 | 06:15:29.7 | -04:54:52.7 | H-coron (~1 hr) | |||||||
HD 43976 | 06:15:38.8 | -57:42:05.5 | H-coron (~1 hr) | |||||||
V* AO Men | 06:18:28.2 | -72:02:41.4 | H-coron (~1 hr) | |||||||
V1358 Ori | 06:19:08.0 | -03:26:20.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 30034 | 06:19:12.9 | -58:03:15.8 | H-coron (~1 hr) | |||||||
HIP 30252 | 06:21:50.0 | -51:14:15.8 | H-coron (~1 hr); H-coron-pol | |||||||
HD 44748 | 06:21:57.2 | -34:30:43.7 | H-coron (~1 hr) | |||||||
HD 45270 | 06:22:31.0 | -60:13:07.7 | H-coron (~1 hr) | |||||||
HIP 30344 | 06:22:57.7 | -24:33:21.6 | H-coron (~1 hr) | |||||||
HIP 30729 | 06:27:20.7 | -33:06:49.9 | H-coron (~1 hr) | |||||||
HIP 31167 | 06:32:23.1 | -05:52:07.4 | H-coron (~1 hr) | |||||||
HIP 31850 | 06:39:31.5 | 24:35:59.8 | H-coron (~1 hr) | |||||||
HIP 31878 | 06:39:50.1 | -61:28:42.2 | H-coron (~1 hr) | |||||||
TYC 4803-141 | 06:40:22.4 | -03:31:59.1 | H-coron (~1 hr) | |||||||
HIP 32075 | 06:42:05.5 | -38:00:13.7 | H-coron (~1 hr) | |||||||
* 26 Gem | 06:42:24.3 | 17:38:43.1 | H-coron (~1 hr) | |||||||
TYC 4803-062 | 06:43:01.0 | -02:53:19.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 32235 | 06:43:46.3 | -71:58:35.8 | H-coron (~1 hr) | |||||||
HIP 32349 | 06:45:08.9 | -16:42:58.0 | H-coron (~1 hr) | |||||||
HD 50571 | 06:50:01.0 | -60:14:57.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 32938 | 06:51:42.5 | -36:13:48.5 | H-coron (~1 hr) | |||||||
HD 50554 | 06:54:42.8 | 24:14:44.0 | H-coron (~1 hr); H-coron-pol | |||||||
HD 51797 | 06:56:23.5 | -46:46:55.0 | H-coron (~1 hr) | |||||||
HD 53143 | 06:59:59.7 | -61:20:10.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 33705 | 07:00:09.8 | -31:08:30.5 | H-coron (~1 hr) | |||||||
HD 55279 | 07:00:30.4 | -79:41:45.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 34271 | 07:06:16.8 | 22:41:00.6 | H-coron (~1 hr) | |||||||
HIP 34782 | 07:12:04.1 | -30:49:17.0 | H-coron (~1 hr) | |||||||
HIP 35350 | 07:18:05.6 | 16:32:25.7 | H-coron (~1 hr) | |||||||
HIP 35564 | 07:20:21.4 | -52:18:41.0 | H-coron (~1 hr) | |||||||
TYC8132-211 | 07:20:21.9 | -52:18:33.3 | H-coron (~1 hr) | |||||||
HIP 35567 | 07:20:23.0 | -56:17:41.3 | H-coron (~1 hr); H-coron-pol | |||||||
TYC 7116-273 | 07:22:16.3 | -35:55:06.6 | H-coron (~1 hr) | |||||||
HIP 35884 | 07:23:53.8 | -17:24:48.2 | H-coron (~1 hr) | |||||||
HIP 36071 | 07:25:57.2 | -02:14:54.5 | H-coron (~1 hr) | |||||||
HD 59704 | 07:29:31.4 | -38:07:21.0 | H-coron (~1 hr) | |||||||
HD 59967 | 07:30:42.6 | -37:20:22.1 | H-coron (~1 hr) | |||||||
HIP 36832 | 07:34:28.0 | -52:58:05.4 | H-coron (~1 hr) | |||||||
HD 61005 | 07:35:47.5 | -32:12:14.7 | H-coron (~1 hr); H-coron-pol | |||||||
TYC 1365-168 | 07:36:01.1 | 18:08:29.5 | H-coron (~1 hr) | |||||||
HIP 37288 | 07:39:23.0 | 02:11:01.2 | H-coron (~1 hr) | |||||||
HD 62237 | 07:42:26.5 | -16:17:00.3 | H-coron (~1 hr) | |||||||
HIP 37563 | 07:42:36.1 | -59:17:51.0 | H-coron (~1 hr) | |||||||
HIP 37718 | 07:44:12.5 | -50:27:24.2 | H-coron (~1 hr) | |||||||
HIP 37727 | 07:44:16.5 | -50:27:59.8 | H-coron (~1 hr) | |||||||
GJ 285 | 07:44:40.2 | 03:33:08.8 | H-coron (~1 hr) | |||||||
HIP 37879 | 07:45:50.9 | -07:31:46.4 | H-coron (~1 hr) | |||||||
HD 63608 | 07:46:17.0 | -59:48:34.0 | H-coron (~1 hr) | |||||||
HR 3070 | 07:49:12.9 | -60:17:01.0 | H-coron (~1 hr) | |||||||
HIP 38188 | 07:49:29.3 | -54:54:04.4 | H-coron (~1 hr) | |||||||
BD +07 1919 | 08:07:09.1 | 07:23:00.1 | H-coron (~1 hr) | |||||||
TYC 0195-257 | 08:11:15.1 | 01:16:36.4 | H-coron (~1 hr) | |||||||
HIP 40706 | 08:18:33.3 | -36:39:33.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 40916 | 08:21:00.5 | -52:13:40.9 | H-coron (~1 hr) | |||||||
HD 70573 | 08:22:50.0 | 01:51:34.0 | H-coron (~1 hr) | |||||||
HIP 41081 | 08:22:55.2 | -52:07:25.6 | H-coron (~1 hr); H-coron-pol | |||||||
V* V592 Pup | 08:25:17.7 | -34:22:01.2 | H-coron (~1 hr) | |||||||
HIP 41373 | 08:26:25.2 | -52:48:27.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 41889 | 08:32:30.5 | 15:49:26.2 | H-coron (~1 hr) | |||||||
HD 72687 | 08:33:15.4 | -29:57:23.8 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 42172 | 08:35:51.0 | 06:37:12.8 | H-coron (~1 hr) | |||||||
V401 Hya | 08:37:50.5 | -06:48:25.2 | H-coron (~1 hr) | |||||||
* eta Cha | 08:41:19.5 | -78:57:48.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 42806 | 08:43:17.2 | 21:28:06.9 | H-coron (~1 hr) | |||||||
HIP 42808 | 08:43:18.0 | -38:52:57.0 | H-coron (~1 hr) | |||||||
HIP 43290 | 08:49:05.7 | -39:57:16.0 | H-coron (~1 hr) | |||||||
HIP 43771 | 08:54:57.2 | -24:23:39.4 | H-coron (~1 hr) | |||||||
HIP 43970 | 08:57:14.9 | 15:19:21.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 44001 | 08:57:35.2 | 15:34:52.6 | H-coron (~1 hr); H-coron-pol | |||||||
TYC 6589-789 | 08:59:18.3 | -24:43:43.9 | H-coron (~1 hr) | |||||||
HIP 44526 | 09:04:20.8 | -15:54:51.0 | H-coron (~1 hr) | |||||||
HIP 45238 | 09:13:12.0 | -69:43:01.9 | H-coron (~1 hr) | |||||||
HIP 45950 | 09:22:17.7 | 06:17:51.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 46422 | 09:27:57.5 | -66:06:07.7 | H-coron (~1 hr) | |||||||
HIP 46634 | 09:30:35.0 | 10:36:00.0 | H-coron (~1 hr) | |||||||
HIP 46816 | 09:32:25.6 | -11:11:04.7 | H-coron (~1 hr) | |||||||
HD 82943 | 09:34:50.7 | -12:07:46.3 | H-coron (~1 hr); H-coron-pol | |||||||
TYC 6601-185 | 09:35:12.2 | -23:50:39.4 | H-coron (~1 hr) | |||||||
TYC 4900-177 | 09:35:12.2 | -05:50:56.6 | H-coron (~1 hr) | |||||||
HD 84075 | 09:36:18.0 | -78:20:42.0 | H-coron (~1 hr); H-coron-pol | |||||||
HD 83946 | 09:38:54.1 | -64:59:26.7 | H-coron (~1 hr) | |||||||
TYC 6606-100 | 09:41:41.9 | -25:57:51.8 | H-coron (~1 hr); H-coron-pol | |||||||
CPD-55 2452B | 09:42:40.6 | -55:49:53.4 | H-coron (~1 hr) | |||||||
HIP 47625A | 09:42:40.8 | -55:49:55.0 | H-coron (~1 hr) | |||||||
HIP 47681 | 09:43:20.3 | -29:48:14.7 | H-coron (~1 hr) | |||||||
BD+17 2140 | 09:49:40.6 | 16:22:13.8 | H-coron (~1 hr) | |||||||
HIP 48273 | 09:50:30.1 | 04:20:37.1 | H-coron (~1 hr) | |||||||
HIP 48341 | 09:51:14.0 | -04:14:35.8 | H-coron (~1 hr) | |||||||
HIP 49165 | 10:02:00.5 | -34:10:25.0 | H-coron (~1 hr) | |||||||
V* AN Sex | 10:12:17.6 | -03:44:44.3 | H-coron (~1 hr) | |||||||
HD 298936 | 10:13:14.7 | -52:30:53.9 | H-coron (~1 hr) | |||||||
HD 88742 | 10:13:24.7 | -33:01:54.2 | H-coron (~1 hr) | |||||||
HIP 50191 | 10:14:44.2 | -42:07:18.9 | H-coron (~1 hr) | |||||||
HIP 50534 | 10:19:16.3 | -11:22:42.2 | H-coron (~1 hr) | |||||||
TYC 0251-101 | 10:19:28.6 | 06:34:59.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 50693 | 10:21:07.9 | -17:59:05.6 | H-coron (~1 hr) | |||||||
HD 90712 | 10:27:47.8 | -34:23:58.1 | H-coron (~1 hr) | |||||||
HIP 51266B | 10:28:17.9 | -52:33:40.0 | H-coron (~1 hr) | |||||||
HIP 51266A | 10:28:18.5 | -52:33:42.0 | H-coron (~1 hr) | |||||||
BD+01 2447 | 10:28:55.5 | 00:50:27.6 | H-coron (~1 hr) | |||||||
HD 90905 | 10:29:42.2 | 01:29:28.0 | H-coron (~1 hr) | |||||||
HIP 51907 | 10:36:17.4 | -10:34:60.0 | H-coron (~1 hr) | |||||||
V* CE Ant | 10:42:30.1 | -33:40:16.2 | H-coron (~1 hr); H-coron-pol | |||||||
V419 Hya | 10:43:28.3 | -29:03:51.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 52787 | 10:47:31.2 | -22:20:52.8 | H-coron (~1 hr) | |||||||
HIP 53217 | 10:53:04.5 | -20:37:41.0 | H-coron (~1 hr) | |||||||
HIP53524 | 10:57:03.1 | -68:40:02.6 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 53771 | 11:00:08.3 | -51:49:04.1 | H-coron (~1 hr) | |||||||
V* TW Hya | 11:01:51.9 | -34:42:17.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 53954 | 11:02:19.8 | 20:10:47.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 54155 | 11:04:41.5 | -04:13:15.9 | H-coron (~1 hr) | |||||||
HIP 54477 | 11:08:44.0 | -28:04:50.2 | H-coron (~1 hr) | |||||||
GJ 1144 | 11:16:22.1 | -14:41:36.1 | H-coron (~1 hr) | |||||||
HIP 55130 | 11:17:12.1 | -38:00:51.8 | H-coron (~1 hr) | |||||||
HIP 55487 | 11:21:49.8 | -24:11:23.0 | H-coron (~1 hr) | |||||||
HD 99827 | 11:25:17.7 | -84:57:16.0 | H-coron (~1 hr) | |||||||
HIP 55943 | 11:27:55.4 | 11:00:36.2 | H-coron (~1 hr) | |||||||
HIP 56367 | 11:33:16.7 | -03:24:08.2 | H-coron (~1 hr) | |||||||
HIP56379 | 11:33:25.5 | -70:11:41.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 56445 | 11:34:22.0 | 03:03:36.6 | H-coron (~1 hr) | |||||||
HIP 57013 | 11:41:19.9 | -43:05:44.4 | H-coron (~1 hr) | |||||||
HIP 57207 | 11:43:49.8 | -35:14:52.8 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 57460 | 11:46:42.3 | -19:28:11.2 | H-coron (~1 hr) | |||||||
HD 102458 | 11:47:24.5 | -49:53:03.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 57562 | 11:47:54.9 | 08:14:45.1 | H-coron (~1 hr) | |||||||
HIP 57632 | 11:49:03.6 | 14:34:19.4 | H-coron (~1 hr) | |||||||
HD 103234 | 11:53:08.0 | -56:43:38.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP58167 | 11:55:43.6 | -54:10:50.4 | H-coron (~1 hr) | |||||||
HIP 58180 | 11:55:57.1 | -77:00:30.2 | H-coron (~1 hr) | |||||||
HIP 58240 | 11:56:42.3 | -32:16:05.4 | H-coron (~1 hr) | |||||||
HIP 58241 | 11:56:43.8 | -32:16:02.7 | H-coron (~1 hr) | |||||||
HIP58465 | 11:59:23.8 | -57:10:04.7 | H-coron (~1 hr) | |||||||
HIP58528 | 12:00:09.4 | -57:07:01.9 | H-coron (~1 hr) | |||||||
HD 104467 | 12:01:39.1 | -78:59:16.9 | H-coron (~1 hr) | |||||||
HIP58720 | 12:02:37.8 | -69:11:32.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP59282 | 12:09:38.8 | -58:20:58.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 59315 | 12:10:06.5 | -49:10:50.7 | H-coron (~1 hr) | |||||||
HIP 59394 | 12:11:03.9 | -23:36:08.5 | H-coron (~1 hr); H-coron-pol | |||||||
HIP59397 | 12:11:05.9 | -56:24:04.8 | H-coron (~1 hr); H-coron-pol | |||||||
HIP59413 | 12:11:14.8 | -52:13:03.1 | H-coron (~1 hr) | |||||||
HIP59481 | 12:11:58.9 | -50:46:12.4 | H-coron (~1 hr) | |||||||
HD 106444 | 12:14:50.7 | -55:47:23.5 | H-coron (~1 hr); H-coron-pol | |||||||
2MASS J1214 | 12:14:52.2 | -55:47:03.7 | H-coron (~1 hr) | |||||||
HIP59724 | 12:14:56.4 | -47:56:54.5 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 59726 | 12:14:57.4 | -41:08:22.0 | H-coron (~1 hr) | |||||||
TWA 25 | 12:15:31 | -39:48:42 | H-coron (~1 hr); H-coron-pol | |||||||
HIP59898 | 12:17:06.4 | -65:41:34.6 | H-coron (~1 hr); H-coron-pol | |||||||
HIP59960 | 12:17:53.2 | -55:58:31.8 | H-coron (~1 hr); H-coron-pol | |||||||
HD 107146 | 12:19:06.5 | 16:32:53.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP60183 | 12:20:28.3 | -65:50:33.5 | H-coron (~1 hr); H-coron-pol | |||||||
HD 107722 | 12:23:29.0 | -77:40:51.0 | H-coron (~1 hr) | |||||||
HIP60459 | 12:23:42.2 | -63:52:12.2 | H-coron (~1 hr) | |||||||
HIP 60595 | 12:25:11.8 | -11:36:37.8 | H-coron (~1 hr) | |||||||
HD 108611 | 12:29:02.2 | -64:55:00.6 | H-coron (~1 hr) | |||||||
HIP61049 | 12:30:46.3 | -58:11:16.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP61087 | 12:31:12.7 | -61:54:31.4 | H-coron (~1 hr) | |||||||
eta CrV | 12:32:04.2 | -16:11:45.6 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 61468 | 12:35:45.6 | -41:01:18.8 | H-coron (~1 hr) | |||||||
HR 4796 | 12:36:01.1 | -39:52:10.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP61684 | 12:38:42.8 | -68:45:49.0 | H-coron (~1 hr); H-coron-pol | |||||||
HD 109908 | 12:38:49.0 | -51:12:56.1 | H-coron (~1 hr); H-coron-pol | |||||||
2MASS J1239 | 12:39:21.2 | -75:02:39.2 | H-coron (~1 hr) | |||||||
HIP61782 | 12:39:46.2 | -49:11:55.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 61960 | 12:41:53.1 | 10:14:08.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP62134 | 12:44:02.0 | -53:30:20.5 | H-coron (~1 hr) | |||||||
HIP 62403 | 12:47:19.0 | -66:14:14.8 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 62482 | 12:48:17 | -67:07:52 | H-coron (~1 hr); H-coron-pol | |||||||
HIP62657 | 12:50:19.8 | -49:51:48.8 | H-coron (~1 hr); H-coron-pol | |||||||
HIP63236 | 12:57:26.3 | -67:57:38.4 | H-coron (~1 hr); H-coron-pol | |||||||
CD-69 1055 | 12:58:25.5 | -70:28:49.2 | H-coron (~1 hr) | |||||||
HIP 63439 | 12:59:59 | -50:23:22 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 63734 | 13:03:39.0 | -16:20:11.7 | H-coron (~1 hr) | |||||||
HIP63836 | 13:04:59.5 | -47:23:48.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 63862 | 13:05:16.8 | -50:51:24.0 | H-coron (~1 hr) | |||||||
HIP 63905 | 13:05:46.3 | -18:49:33.0 | H-coron (~1 hr) | |||||||
HD 113853 | 13:06:59.1 | -37:44:40.1 | H-coron (~1 hr) | |||||||
HIP64184 | 13:09:16.2 | -60:18:29.9 | H-coron (~1 hr); H-coron-pol | |||||||
HD 114613 | 13:12:03.2 | -37:48:11.0 | H-coron (~1 hr) | |||||||
HD 115383 | 13:16:46.5 | 09:25:27.0 | H-coron (~1 hr) | |||||||
HIP 64822 | 13:17:13.9 | -43:58:46.0 | H-coron (~1 hr) | |||||||
61 Vir | 13:18:24.3 | -18:18:40.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP64995 | 13:19:19.6 | -59:28:20.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP65089 | 13:20:26.8 | -49:13:25.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 65109 | 13:20:35.8 | -36:42:44.3 | H-coron (~1 hr) | |||||||
HIP 65198 | 13:21:41.6 | 02:05:14.1 | H-coron (~1 hr) | |||||||
HIP 65208 | 13:21:49.8 | -36:06:44.0 | H-coron (~1 hr) | |||||||
HIP65875 | 13:30:09.0 | -58:29:04.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP65965 | 13:31:31.0 | -46:44:06.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 66065 | 13:32:36.0 | -28:41:33.8 | H-coron (~1 hr) | |||||||
HIP 66121 | 13:33:13.7 | -77:34:09.8 | H-coron (~1 hr) | |||||||
HIP 66200 | 13:34:07.9 | 03:39:32.5 | H-coron (~1 hr) | |||||||
HIP66454 | 13:37:23.5 | -46:25:40.2 | H-coron (~1 hr) | |||||||
HIP66722 | 13:40:37.7 | -44:19:48.7 | H-coron (~1 hr) | |||||||
HIP66821 | 13:41:44.8 | -54:33:33.7 | H-coron (~1 hr) | |||||||
TYC 8262-204 | 13:43:22.0 | -46:38:08.6 | H-coron (~1 hr) | |||||||
HIP67199 | 13:46:14.5 | -54:40:59.9 | H-coron (~1 hr) | |||||||
HIP67497 | 13:49:54.5 | -50:14:23.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP67957 | 13:55:01.3 | -50:45:01.9 | H-coron (~1 hr) | |||||||
G 150-52 | 13:57:16.1 | 23:21:44.3 | H-coron (~1 hr); H-coron-pol | |||||||
TYC 1470-000 | 13:58:13.6 | 19:17:11.9 | H-coron (~1 hr) | |||||||
HIP68335 | 13:59:18.1 | -51:53:34.0 | H-coron (~1 hr) | |||||||
HIP68781 | 14:04:42.2 | -50:04:16.9 | H-coron (~1 hr); H-coron-pol | |||||||
HD 122973 | 14:05:10.6 | -09:02:54.6 | H-coron (~1 hr) | |||||||
HIP 68994 | 14:07:29.3 | -61:33:43.9 | H-coron (~1 hr) | |||||||
HIP 69592 | 14:14:40.9 | 21:52:24.3 | H-coron (~1 hr) | |||||||
HIP 69751 | 14:16:32.8 | 20:07:18.7 | H-coron (~1 hr) | |||||||
HIP 69781 | 14:16:57.9 | -49:56:42.0 | H-coron (~1 hr) | |||||||
HD 125283 | 14:19:23.9 | -37:00:10.1 | H-coron (~1 hr) | |||||||
HD 125485 | 14:23:39.1 | -72:48:29.5 | H-coron (~1 hr) | |||||||
HD 126246 B | 14:24:05.4 | 11:14:57.8 | H-coron (~1 hr) | |||||||
TYC 0912-157 | 14:24:05.5 | 11:14:57.5 | H-coron (~1 hr) | |||||||
HIP70441 | 14:24:37.0 | -47:10:39.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP70558 | 14:25:58.5 | -44:49:23.2 | H-coron (~1 hr) | |||||||
HIP70689 | 14:27:30.5 | -52:31:30.2 | H-coron (~1 hr) | |||||||
HIP70697 | 14:27:33.6 | -46:12:48.5 | H-coron (~1 hr) | |||||||
HIP70833 | 14:29:07.2 | -43:21:42.6 | H-coron (~1 hr) | |||||||
HIP71271 | 14:34:33.5 | -46:18:17.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP71321 | 14:35:05.4 | -43:33:16.1 | H-coron (~1 hr) | |||||||
HIP 71743 | 14:40:31.1 | -16:12:33.4 | H-coron (~1 hr) | |||||||
HIP 71855 | 14:41:52.5 | -75:08:22.0 | H-coron (~1 hr) | |||||||
HIP 71899 | 14:42:23.1 | 21:17:35.1 | H-coron (~1 hr) | |||||||
HD 129181 | 14:42:43.5 | -48:47:58.6 | H-coron (~1 hr) | |||||||
HIP 72070 | 14:44:31 | -39:59:21 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 72048 | 14:44:14.1 | -69:40:26.8 | H-coron (~1 hr) | |||||||
HD 129679 | 14:44:16.8 | -11:37:02.4 | H-coron (~1 hr) | |||||||
HIP 72197B | 14:46:00.6 | -25:26:39.9 | H-coron (~1 hr) | |||||||
HIP72627 | 14:50:58.7 | -42:49:20.8 | H-coron (~1 hr) | |||||||
HD 131435 | 14:54:54.8 | -41:21:53.1 | H-coron (~1 hr) | |||||||
HD 130943 | 14:55:46.1 | -73:09:59.8 | H-coron (~1 hr) | |||||||
HIP73145 | 14:56:54.5 | -35:41:43.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP73266 | 14:58:24.3 | -37:21:44.7 | H-coron (~1 hr) | |||||||
HD 132173 | 14:58:30.5 | -28:42:34.3 | H-coron (~1 hr) | |||||||
HD 133295 | 15:04:33.1 | -28:18:00.2 | H-coron (~1 hr) | |||||||
HIP73990 | 15:07:15.0 | -29:30:15.9 | H-coron (~1 hr); H-coron-pol | |||||||
BD+09 3000A | 15:07:32.9 | 09:13:33.7 | H-coron (~1 hr) | |||||||
HIP 74049 | 15:07:57.8 | -45:34:45.9 | H-coron (~1 hr) | |||||||
HIP 74380 | 15:11:57.7 | -48:44:37.3 | H-coron (~1 hr) | |||||||
V* NY Aps | 15:12:23.4 | -75:15:15.6 | H-coron (~1 hr) | |||||||
HIP 74493 | 15:13:19.2 | -19:38:51.0 | H-coron (~1 hr) | |||||||
HIP74499 | 15:13:28.0 | -33:08:50.0 | H-coron (~1 hr); H-coron-pol | |||||||
HD 135271 | 15:15:13.9 | -30:58:40.1 | H-coron (~1 hr) | |||||||
HIP 74689 | 15:15:49.1 | 00:22:19.6 | H-coron (~1 hr) | |||||||
HIP 74696 | 15:15:53.7 | -48:04:25.1 | H-coron (~1 hr) | |||||||
HIP 74824 | 15:17:30.9 | -58:48:04.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP74865 | 15:17:56.1 | -30:28:41.2 | H-coron (~1 hr) | |||||||
HIP 74931 | 15:18:42.2 | 10:25:26.7 | H-coron (~1 hr) | |||||||
HIP 74946 | 15:18:54.7 | -68:40:46.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP74959 | 15:19:05.4 | -36:21:44.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP75077 | 15:20:31.4 | -28:17:13.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP75210 | 15:22:11.3 | -37:38:08.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 75379 | 15:24:11.9 | -10:19:20.2 | H-coron (~1 hr) | |||||||
HIP75480 | 15:25:09.4 | -26:34:30.7 | H-coron (~1 hr) | |||||||
HIP75915 | 15:30:21.3 | -41:55:08.3 | H-coron (~1 hr) | |||||||
HIP 76028 | 15:31:42.6 | -20:09:51.8 | H-coron (~1 hr) | |||||||
HIP 76063 | 15:32:04.2 | -38:37:21.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP76084 | 15:32:20.2 | -31:08:33.7 | H-coron (~1 hr) | |||||||
CD-51 9202 | 15:32:36.7 | -52:21:20.7 | H-coron (~1 hr) | |||||||
HIP 76276 | 15:34:48.1 | 10:32:19.9 | H-coron (~1 hr) | |||||||
HIP 76310 | 15:35:16 | -25:44:03 | H-coron (~1 hr); H-coron-pol | |||||||
V343 Nor | 15:38:57.5 | -57:42:27.3 | H-coron (~1 hr) | |||||||
HIP76633 | 15:39:00.1 | -19:43:57.0 | H-coron (~1 hr) | |||||||
g Lup | 15:41:11.4 | -44:39:40.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP76875 | 15:41:53.2 | -34:53:19.6 | H-coron (~1 hr) | |||||||
HIP 77310 | 15:47:00.2 | -62:47:47.6 | H-coron (~1 hr) | |||||||
HIP77317 | 15:47:06.2 | -35:31:04.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP77432 | 15:48:24.8 | -42:37:04.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 77464 | 15:48:56.8 | -03:49:06.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP77520 | 15:49:39.7 | -38:46:38.7 | H-coron (~1 hr) | |||||||
HIP 77541 | 15:49:57.5 | -48:54:44.7 | H-coron (~1 hr) | |||||||
HD 141569 | 15:49:57.8 | -03:55:16.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP77545 | 15:49:59.8 | -25:09:03.4 | H-coron (~1 hr) | |||||||
HIP 77622 | 15:50:49.0 | 04:28:39.8 | H-coron (~1 hr) | |||||||
NZ Lup | 15:53:27.3 | -42:16:00.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP77911 | 15:54:41.6 | -22:45:58.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP78043 | 15:56:05.6 | -36:53:34.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 78045 | 15:56:06.0 | -60:28:56.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP78099 | 15:56:47.9 | -23:11:02.5 | H-coron (~1 hr) | |||||||
HD 142415 | 15:57:40.8 | -60:12:01.0 | H-coron (~1 hr) | |||||||
HIP78196 | 15:57:59.4 | -31:43:43.9 | H-coron (~1 hr) | |||||||
HIP78207 | 15:58:11.4 | -14:16:45.5 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 78343 | 15:59:47.7 | -35:50:43.0 | H-coron (~1 hr) | |||||||
HIP 78553 | 16:02:16.1 | -73:30:54.8 | H-coron (~1 hr) | |||||||
HIP78555 | 16:02:18.5 | -35:16:11.5 | H-coron (~1 hr) | |||||||
HIP78641 | 16:03:13.6 | -35:17:14.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP78663 | 16:03:33.4 | -30:08:13.2 | H-coron (~1 hr) | |||||||
TYC 0945-080 | 16:06:10.3 | 08:35:44.4 | H-coron (~1 hr) | |||||||
HIP78996 | 16:07:29.9 | -23:57:02.2 | H-coron (~1 hr); H-coron-pol | |||||||
HD 145229 | 16:09:26.6 | 11:34:28.1 | H-coron (~1 hr) | |||||||
HIP 79203 | 16:09:55.3 | -18:20:26.2 | H-coron (~1 hr) | |||||||
HIP79288 | 16:10:55.1 | -25:31:21.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP79410 | 16:12:21.8 | -19:34:44.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP79516 | 16:13:34.4 | -45:49:03.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP79599 | 16:14:28.9 | -21:06:27.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 79730 | 16:16:19.6 | -01:38:53.3 | H-coron (~1 hr) | |||||||
HIP79742 | 16:16:28.4 | -38:44:12.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 79797 | 16:17:05.5 | -67:56:28.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 79881 | 16:18:17.9 | -28:36:50.5 | H-coron (~1 hr); H-coron-pol | |||||||
HD 146610 | 16:18:38.5 | -38:39:11.8 | H-coron (~1 hr) | |||||||
HIP 79958 | 16:19:15.9 | -55:30:17.0 | H-coron (~1 hr) | |||||||
HIP79977 | 16:19:29.3 | -21:24:13.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 80065 | 16:20:32.5 | -45:48:35.0 | H-coron (~1 hr) | |||||||
HIP80088 | 16:20:50.2 | -22:35:38.6 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 80170 | 16:21:55.2 | 19:09:10.9 | H-coron (~1 hr) | |||||||
HIP80324 | 16:23:56.7 | -33:11:57.6 | H-coron (~1 hr) | |||||||
HD 147513 | 16:24:01.3 | -39:11:35.0 | H-coron (~1 hr) | |||||||
TYC 0959-098 | 16:26:48.9 | 08:23:26.0 | H-coron (~1 hr) | |||||||
HIP80591 | 16:27:14.6 | -39:49:21.7 | H-coron (~1 hr) | |||||||
TYC 5626-097 | 16:27:29.0 | -08:34:19.2 | H-coron (~1 hr) | |||||||
HIP 80686 | 16:28:28.1 | -70:05:03.8 | H-coron (~1 hr) | |||||||
HIP 81068 | 16:33:30.1 | 17:49:43.2 | H-coron (~1 hr) | |||||||
HIP 81425 | 16:37:48.0 | 13:41:13.9 | H-coron (~1 hr) | |||||||
HIP 81592 | 16:39:47.0 | -51:59:39.0 | H-coron (~1 hr) | |||||||
HD 150554 | 16:40:56.5 | 21:56:53.3 | H-coron (~1 hr) | |||||||
HIP 82303 | 16:48:59.8 | -08:55:47.7 | H-coron (~1 hr) | |||||||
HD 151798 | 16:50:05.2 | -12:23:14.8 | H-coron (~1 hr) | |||||||
HIP82397 | 16:50:10.7 | -26:44:32.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP82534 | 16:52:13.3 | -26:55:10.6 | H-coron (~1 hr) | |||||||
HD 152555 | 16:54:08.1 | -04:20:24.7 | H-coron (~1 hr) | |||||||
HIP 82747 | 16:54:45 | -36:53:19 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 83187 | 17:00:06.2 | -54:35:49.2 | H-coron (~1 hr); H-coron-pol | |||||||
BD+07 3306B | 17:06:56.7 | 06:47:48.1 | H-coron (~1 hr) | |||||||
HD 154734 | 17:06:57.5 | 06:48:02.9 | H-coron (~1 hr) | |||||||
HIP 83962 | 17:09:48.0 | -10:31:23.9 | H-coron (~1 hr) | |||||||
HIP 84121 | 17:11:51.2 | -45:52:27.6 | H-coron (~1 hr) | |||||||
HIP 84150 | 17:12:16.2 | -39:30:24.4 | H-coron (~1 hr) | |||||||
HIP 84229B | 17:12:58.9 | -58:35:47.0 | H-coron (~1 hr) | |||||||
HIP 84397 | 17:15:17.3 | -07:12:06.0 | H-coron (~1 hr) | |||||||
HIP 84586 | 17:17:25.5 | -66:57:03.7 | H-coron (~1 hr) | |||||||
HIP 84881 | 17:20:51 | -45:25:15 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 85038 | 17:22:47.9 | -58:28:23.7 | H-coron (~1 hr) | |||||||
HIP 85157 | 17:24:06.6 | 22:57:37.4 | H-coron (~1 hr); H-coron-pol | |||||||
HD 157587 | 17:24:52.2 | -18:51:33.2 | H-coron (~1 hr); H-coron-pol | |||||||
TYC 7883-206 | 17:25:34.3 | -38:48:39.7 | H-coron (~1 hr) | |||||||
HIP 85307 | 17:25:57.8 | -01:39:06.8 | H-coron (~1 hr) | |||||||
HIP 85360 | 17:26:34.9 | -32:58:11.0 | H-coron (~1 hr) | |||||||
CD-54 7336 | 17:29:55.0 | -54:15:48.6 | H-coron (~1 hr) | |||||||
HIP 85922 | 17:33:29.9 | -05:44:40.5 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 86305 | 17:38:05.5 | -54:30:01.6 | H-coron (~1 hr); H-coron-pol | |||||||
HD 160305 | 17:41:49.0 | -50:43:28.0 | H-coron (~1 hr) | |||||||
HIP 86672 | 17:42:30.4 | -28:44:56.0 | H-coron (~1 hr) | |||||||
TYC 0424-195 | 17:46:25.4 | 03:58:48.9 | H-coron (~1 hr) | |||||||
HD 161012 | 17:46:48.5 | -59:06:14.7 | H-coron (~1 hr) | |||||||
HIP 87108 | 17:47:53.6 | 02:42:26.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 87914A | 17:57:31.7 | -57:39:51.0 | H-coron (~1 hr) | |||||||
HD 164249 | 18:03:03.4 | -51:38:55.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 88694 | 18:06:23.7 | -36:01:11.0 | H-coron (~1 hr) | |||||||
HIP 89805 | 18:19:40.1 | -63:53:11.6 | H-coron (~1 hr) | |||||||
HIP 90133 | 18:23:36.4 | -75:02:39.6 | H-coron (~1 hr) | |||||||
TYC 7401-244 | 18:24:50.6 | -34:11:26.4 | H-coron (~1 hr) | |||||||
L 206-187 | 18:30:11.9 | -58:16:27.6 | H-coron (~1 hr) | |||||||
HD 170773 | 18:33:00.9 | -39:53:31.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 90991 | 18:33:39.0 | -14:51:12.9 | H-coron (~1 hr) | |||||||
HIP 91043 | 18:34:20.2 | 18:41:24.7 | H-coron (~1 hr) | |||||||
HIP 91217 | 18:36:27.8 | 09:07:21.0 | H-coron (~1 hr) | |||||||
HIP 92024 | 18:45:26.9 | -64:52:16.5 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 92161 | 18:47:01.3 | 18:10:53.5 | H-coron (~1 hr) | |||||||
PZ Tel | 18:53:05.9 | -50:10:50.0 | H-coron (~1 hr) | |||||||
HIP 92871 | 18:55:27.4 | 08:24:09.6 | H-coron (~1 hr) | |||||||
HD 175726 | 18:56:37.2 | 04:15:55.2 | H-coron (~1 hr) | |||||||
HIP 93375 | 19:01:06.0 | -28:42:49.7 | H-coron (~1 hr) | |||||||
HD 176383 | 19:01:28.6 | -34:22:35.5 | H-coron (~1 hr); H-coron-pol | |||||||
TYC 466-1374 | 19:02:17.1 | 02:44:22.0 | H-coron (~1 hr) | |||||||
rho Tel | 19:06:19.9 | -52:20:26.3 | H-coron (~1 hr) | |||||||
HIP 94020 | 19:08:31.7 | -30:58:21.1 | H-coron (~1 hr) | |||||||
HIP 94050 | 19:08:50.5 | -42:25:41.0 | H-coron (~1 hr) | |||||||
HIP 94114 | 19:09:28.3 | -37:54:16.1 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 95261 | 19:22:51.2 | -54:25:26.2 | H-coron (~1 hr); H-coron-pol | |||||||
HD 181327 | 19:22:58.9 | -54:32:17.0 | H-coron (~1 hr); H-coron-pol | |||||||
HD 181869 | 19:23:53.2 | -40:36:57.4 | H-coron (~1 hr) | |||||||
HD 182681 | 19:26:56.5 | -29:44:35.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 95793 | 19:29:01.0 | 01:57:01.9 | H-coron (~1 hr) | |||||||
HD 183216 | 19:29:40.6 | -30:47:51.9 | H-coron (~1 hr); H-coron-pol | |||||||
TYC 7429-169 | 19:30:57.4 | -32:41:56.7 | H-coron (~1 hr) | |||||||
HIP 96334 | 19:35:09.7 | -69:58:32.0 | H-coron (~1 hr) | |||||||
HD 185181 | 19:38:51.5 | -25:52:19.5 | H-coron (~1 hr) | |||||||
HIP 96880 | 19:41:35.7 | -72:26:45.7 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 97229 | 19:45:39.9 | 07:36:47.4 | H-coron (~1 hr) | |||||||
HIP 97423 | 19:48:03.0 | -13:42:12.8 | H-coron (~1 hr) | |||||||
HIP 97557 | 19:49:44.0 | -32:45:49.7 | H-coron (~1 hr) | |||||||
HIP 97944 | 19:54:17.8 | -23:56:27.9 | H-coron (~1 hr) | |||||||
HIP 98470 | 20:00:20.3 | -33:42:12.4 | H-coron (~1 hr) | |||||||
HD 188228 | 20:00:35.6 | -72:54:37.8 | H-coron (~1 hr) | |||||||
CD-50 12781 | 20:02:36.2 | -50:03:00.3 | H-coron (~1 hr) | |||||||
HIP 98839 | 20:04:18.1 | -26:19:46.3 | H-coron (~1 hr) | |||||||
HD 190081 | 20:04:36.5 | -35:12:51.1 | H-coron (~1 hr) | |||||||
TYC 9098-129 | 20:07:19.8 | -65:51:08.8 | H-coron (~1 hr) | |||||||
HD 191089 | 20:09:05.2 | -26:13:26.5 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 99742 | 20:14:16.6 | 15:11:50.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 99803 | 20:14:56.1 | -56:58:34.5 | H-coron (~1 hr) | |||||||
CPD-57 9635B | 20:14:56.4 | -56:58:28.8 | H-coron (~1 hr) | |||||||
HD 193924 | 20:25:38.9 | -56:44:05.6 | H-coron (~1 hr) | |||||||
HIP 100787 | 20:26:04.7 | -46:39:35.8 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 101022 | 20:28:49.9 | -01:44:04.1 | H-coron (~1 hr) | |||||||
HIP 101120 | 20:29:52.6 | -18:35:10.3 | H-coron (~1 hr) | |||||||
HIP 101123 | 20:29:53.9 | -18:34:59.5 | H-coron (~1 hr) | |||||||
HIP 101483 | 20:33:57.0 | 13:01:37.9 | H-coron (~1 hr) | |||||||
HD 195830 | 20:34:46.9 | -33:55:19.0 | H-coron (~1 hr) | |||||||
HD 195627 | 20:35:34.9 | -60:34:54.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 101800 | 20:37:49.1 | 11:22:39.7 | H-coron (~1 hr); H-coron-pol | |||||||
AU Mic | 20:45:09.5 | -31:20:27.2 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 102531 | 20:46:38.9 | 16:07:26.9 | H-coron (~1 hr) | |||||||
V* BO Mic | 20:47:45.0 | -36:35:40.7 | H-coron (~1 hr) | |||||||
CD-28 16938 | 20:49:47.9 | -28:28:09.1 | H-coron (~1 hr) | |||||||
HIP 103107 | 20:53:25.9 | -49:22:58.1 | H-coron (~1 hr) | |||||||
HD 199260 | 20:56:47.3 | -26:17:46.4 | H-coron (~1 hr) | |||||||
HD 199065A | 20:57:22.4 | -59:04:33.4 | H-coron (~1 hr) | |||||||
HIP 103460 | 20:57:40.6 | -16:01:53.6 | H-coron (~1 hr) | |||||||
HIP 104239 | 21:07:10.4 | -13:55:23.0 | H-coron (~1 hr) | |||||||
HIP 104308 | 21:07:51.2 | -54:12:58.8 | H-coron (~1 hr) | |||||||
HIP 104365 | 21:08:33.6 | -21:11:36.6 | H-coron (~1 hr) | |||||||
HIP 104526A | 21:10:25.4 | -54:34:26.0 | H-coron (~1 hr) | |||||||
TYC 8797-137 | 21:10:25.7 | -54:34:28.1 | H-coron (~1 hr) | |||||||
HIP 104687B | 21:12:22.4 | -14:59:58.0 | H-coron (~1 hr) | |||||||
HIP 104687A | 21:12:22.6 | -15:00:00.0 | H-coron (~1 hr) | |||||||
HIP 104864 | 21:14:32.8 | -22:52:41.1 | H-coron (~1 hr) | |||||||
HIP 105044 | 21:16:37.9 | -36:10:24.1 | H-coron (~1 hr) | |||||||
HIP 105156 | 21:18:05.2 | -29:30:48.2 | H-coron (~1 hr) | |||||||
HIP 105184 | 21:18:27.3 | -43:20:05.0 | H-coron (~1 hr) | |||||||
HD 202917 | 21:20:49.9 | -53:02:02.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 105404 | 21:20:59.8 | -52:28:40.1 | H-coron (~1 hr) | |||||||
HIP 105441 | 21:21:24.5 | -66:54:57.4 | H-coron (~1 hr) | |||||||
HIP 105612 | 21:23:27.1 | -75:29:38.6 | H-coron (~1 hr) | |||||||
HIP 105712 | 21:24:40.6 | -68:13:40.2 | H-coron (~1 hr) | |||||||
HIP 105860 | 21:26:26.6 | 19:22:32.2 | H-coron (~1 hr) | |||||||
HD 205674 | 21:37:21.1 | -18:26:28.2 | H-coron (~1 hr); H-coron-pol | |||||||
HD 205905 | 21:39:10.2 | -27:18:24.0 | H-coron (~1 hr) | |||||||
HIP 107095 | 21:41:32.9 | -14:02:51.4 | H-coron (~1 hr) | |||||||
HN Peg | 21:44:31.3 | 14:46:19.0 | H-coron (~1 hr) | |||||||
HD 206893 | 21:45:21.9 | -12:47:00.0 | H-coron (~1 hr); H-coron-pol | |||||||
HD 207129 | 21:48:15.8 | -47:18:13.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 107947 | 21:52:09.7 | -62:03:08.5 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 108060 | 21:53:37.4 | 19:40:06.2 | H-coron (~1 hr) | |||||||
HIP 108405 | 21:57:41.2 | -51:00:22.0 | H-coron (~1 hr) | |||||||
HD 209253 | 22:02:33.0 | -32:08:01.5 | H-coron (~1 hr); H-coron-pol | |||||||
HD 209100 | 22:03:21.7 | -56:47:10.0 | H-coron (~1 hr) | |||||||
HIP 108912 | 22:03:42.4 | -60:26:15.0 | H-coron (~1 hr) | |||||||
HD 209952 | 22:08:14.0 | -46:57:39.5 | H-coron (~1 hr) | |||||||
HIP 109285 | 22:08:23.0 | -32:59:18.2 | H-coron (~1 hr) | |||||||
V* CS Gru | 22:15:35.2 | -39:00:50.6 | H-coron (~1 hr) | |||||||
BD-14 6241 | 22:16:00.6 | -14:11:02.3 | H-coron (~1 hr) | |||||||
HIP 110935 | 22:28:37.7 | -67:29:20.6 | H-coron (~1 hr) | |||||||
HIP 111188 | 22:31:30.3 | -32:20:45.7 | H-coron (~1 hr); H-coron-pol | |||||||
39 Peg | 22:32:35.5 | 20:13:48.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 111594 | 22:36:29.3 | -40:34:57.0 | H-coron (~1 hr) | |||||||
HD 214867 | 22:41:45.4 | -39:27:41.9 | H-coron (~1 hr) | |||||||
CPD-72 2713 | 22:42:48.9 | -71:42:21.2 | H-coron (~1 hr) | |||||||
TYC 1701-064 | 22:44:41.5 | 17:54:18.3 | H-coron (~1 hr) | |||||||
V* WW PsA | 22:44:57.9 | -33:15:01.7 | H-coron (~1 hr) | |||||||
HIP 112515 | 22:47:26.7 | -44:57:55.0 | H-coron (~1 hr) | |||||||
HIP 112581 | 22:48:06.9 | -37:45:24.0 | H-coron (~1 hr) | |||||||
HIP 112714 | 22:49:32.2 | 10:28:43.3 | H-coron (~1 hr) | |||||||
TW PsA | 22:56:24.1 | -31:33:56.0 | H-coron (~1 hr) | |||||||
Fomalhaut | 22:57:39.0 | -29:37:20.0 | H-coron (~1 hr); H-coron-pol | |||||||
HD 217343 | 23:00:19.3 | -26:09:13.5 | H-coron (~1 hr) | |||||||
MT Peg | 23:03:05.0 | 20:55:06.9 | H-coron (~1 hr) | |||||||
HIP 113839 | 23:03:11.6 | -47:15:19.1 | H-coron (~1 hr) | |||||||
HR 8799 | 23:07:28.7 | 21:08:03.3 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 114530 | 23:11:52.1 | -45:08:10.0 | H-coron (~1 hr) | |||||||
HIP 114948 | 23:16:57.7 | -62:00:04.3 | H-coron (~1 hr) | |||||||
HIP 115527 | 23:24:06.3 | -07:33:03.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 115738 | 23:26:56.0 | 01:15:20.2 | H-coron (~1 hr); H-coron-pol | |||||||
CD-86 147 | 23:27:49.4 | -86:13:18.7 | H-coron (~1 hr) | |||||||
GJ 1284 | 23:30:13.4 | -20:23:27.4 | H-coron (~1 hr) | |||||||
HIP 116063 | 23:31:02.9 | -69:04:36.3 | H-coron (~1 hr) | |||||||
TYC 5835-023 | 23:32:22.7 | -13:39:07.0 | H-coron (~1 hr) | |||||||
BD-13 6424 | 23:32:30.8 | -12:15:51.4 | H-coron (~1 hr) | |||||||
HIP 116258 | 23:33:23.8 | -12:39:53.0 | H-coron (~1 hr) | |||||||
HD 221853 | 23:35:36.2 | 08:22:57.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 116611 | 23:37:56.8 | 18:24:02.2 | H-coron (~1 hr) | |||||||
2MASS J2339 | 23:39:39.2 | -69:11:39.5 | H-coron (~1 hr) | |||||||
TYC 9339-551 | 23:39:39.4 | -69:11:44.8 | H-coron (~1 hr) | |||||||
HIP 116928 | 23:42:02.8 | 01:46:48.1 | H-coron (~1 hr) | |||||||
HIP 116971 | 23:42:43.3 | -14:32:41.7 | H-coron (~1 hr) | |||||||
HIP 117219 | 23:46:01.2 | -40:10:56.9 | H-coron (~1 hr) | |||||||
HIP 117452 | 23:48:55.6 | -28:07:49.0 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 117481 | 23:49:19.6 | -27:51:14.9 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 118008 | 23:56:10.7 | -39:03:08.4 | H-coron (~1 hr); H-coron-pol | |||||||
HIP 118121 | 23:57:35.0 | -64:17:53.1 | H-coron (~1 hr) |
GPI News Email Exploder
If you wish to receive news from GPI and any updates from the GPI webpages, you can subscribe to the email exploder : gpinews@gemini.edu.
To subscribe to the list, click on Subscribe. This will send a message to listserver@gemini.edu with a subject of "subscribe gpinews" (without the quotation marks).
To leave this list at any time, click on Unsubscribe. This will send email to with a subject of "unsubscribe gpinews" (without the quotation marks).
GPI Public Data
Several GPI raw and reduced datasets are available as part of a First Data Release.
Information about these datasets are presented in the Table below, with links to download the datasets.
Anyone downloading any of the datasets should read the GPI Public Data Early Release Readme as it contains vital information.
If you use any of these data in a publication, please include the standard Gemini acknowledgment:
Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério Ciência, Tecnologia e Inovação (Brazil) and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina).
Flats and Arcs can be found at :
Raw | Reduced | Information |
CALIB_Y_raw.tar | CALIB_Y_reduced.tar | Flats and Ar Arcs in Y band |
CALIB_J_raw.tar | CALIB_J_reduced.tar | Flats and Ar Arcs in J band |
CALIB_H_raw.tar | CALIB_H_reduced.tar | Flats and Ar Arcs in H band |
CALIB_K1_raw.tar | CALIB_K1_reduced.tar | Flats and Ar Arcs in K1 band |
CALIB_K2_raw.tar | CALIB_K2_reduced.tar | Flats and Ar, Xe Arcs in K2 band |
The dark package is available at : Darks.zip, the wavelength reference calibration package at : Wavecals.zip, the distortion map at: S20120121210S0066-distor-150310.fits.gz, the badPixelmap at: BadPixelMaps.tar.gz and the lenslet flat at: S20131212S0004_lensletflat_spec.fits.gz .
The current version of the GPI IDL pipeline and data reduction package is now available from the instrument build team.
Recipes are available here : extract_recipes.py
GPIES Campaign
Gemini Planet Imager Extra Solar Survey
The GPIES Campaign is the winning proposal in the CfP for Campaign observations with GPI. It was awarded 890h over six semesters starting in 2014B and concluded in semester 2018B.
GPIES Campaign Executive summary
Program Time usage of the GPIES Campaign
GPIES Observations in the Gemini Observatory Archive (GOA)
GPIES Campaign Executive summary
The Gemini Planet Imager (GPI) was built as a survey instrument to directly detect planets and image debris disks. Our survey will use GPI to produce the first-ever robust census of giant planet populations in the 5-50 AU range, allowing us to
- formation pathways of Jovian planets
- early dynamical evolution of systems, including migration mechanisms and the interaction with disks and belts of debris
- gap between Jupiter and the brown dwarfs with the first examples of cool planetary atmospheres.
The only way to achieve robust and reliable statistical results is with a single coherent survey, with uniform and well-articulated selection criteria. We will observe 600 stars spanning spectral types A-M. We will use published young association catalogs and a proprietary list – the result of thousands of hours of telescope observations in preparation for GPI—that adds several hundred new young (<100 Myr, <75 and adolescent (<300 Myr, <35 stars. The latter, closer than the known young associations, allow our survey to probe the 5 AU ice line. Monte Carlo simulations of populations around these stars allow us to optimize the survey strategy for maximum statistical yield. The range of separations studied by GPI is completely inaccessible to Doppler and transit techniques (even with Kepler—a new window into planet formation.
this survey will discover approximately 50 increasing the number of images by an order of magnitude, enough for statistical investigation. The survey will deliver:
- A catalog of —the principal legacy of this campaign—released for follow-up to the Gemini community within 18 months of observation
- For a subset of 10 planets, a library of high-SNR GPI spectra at all 5 bands to calibrate temperature and gravity indicators
- For each planet, estimated effective temperatures and luminosities from GPI spectrophotometry, and semi-major axis estimates from orbital motion
- Empirical measurements of the number of young planets as a function of mass, semi-major axis, and stellar mass with the same precision as Doppler giant-planet surveys
- An estimated eccentricity distribution of a subset of planets sufficient to distinguish different dynamical evolutionary states at the 3-5 sigma level
- 6. Snapshot images of those stars in the survey predicted to have detectable debris disks
- High-SNR images of all debris disks showing planet-induced structure
- An automated data pipeline to process images and recover calibrated astrometry and photometry
- A public catalog containing all reduced images, recovered planetary properties, and detection limits
The large sample will for the first time match the statistical power of extant studies of planets using indirect techniques. GPI spectroscopy will reveal atmospheric conditions and thermal history, thereby calibrating atmosphere and accretion models. The statistical properties of the distributions will arbitrate between various formation and migration scenarios.
Program Time usage of the GPIES Campaign
Total allocation is 890 hours over 6 semesters, starting semester 2014B
Semester |
Hours |
Nights |
Night Hours |
Comments |
Scheduled |
Scheduled |
|||
2014B |
73.5 |
19 |
190 |
Programs GS-2014B-Q-500 and GS-2014B-Q-501 |
2015A |
97.5 |
20 |
200 |
Programs GS-2015A-Q-500 and GS-2015A-Q-501 |
2015B |
99 |
24 |
240 |
Programs GS-2015B-Q-500 and GS-2015B-Q-501 |
2016A |
113.7 |
26 |
260 |
Continued use of 15B programs |
2016B |
105.9 |
26 |
260 |
Continued use of 15B programs |
2017A |
48 |
20 |
200 |
Continued use of 15B programs |
2017B |
120.5 |
28 |
280 |
Programs GS-2017B-Q-500 and GS-2017B-Q-501 |
TOTAL |
658.1 |
160 |
1600 |
UpdatedFebruary 28th, 2018 74% progress on allocated time* 41% Effectiveness (IQ70 CC50 constraints expected 35%) ** |
*Progress is the percentage of the progress in completing the allocated 890h
**Percentage is the ratio of "Charged Time" to "Allocated Night hours"
GPIES Observations in the Gemini Observatory Archive (GOA)
The Gemini Observatory Archive contains all GPIES observations. It should be noted that observations have the same proprietary period as regular queue. Any observation that is still will only be not have any links available for download. link to the observations can be found here:
GS-2014B-Q-500 Data for semester 2014B
GS-2014B-Q-501 Data for semester 2014B
GS-2015A-Q-500 Data for semester 2015A
GS-2015A-Q-501 Data for semester 2015A
GS-2015B-Q-500 data from August 1st, 2015 to January 31st 2016
GS-2015B-Q-501 data from August 1st, 2015 to January 31st 2016
GS-2015B-Q-500 data from February 1st, 2016 to July 31st 2016
GS-2015B-Q-501 data from February 1st, 2016 to July 31st 2016
GS-2015B-Q-500 data from August 1st, 2016 to January 31st, 2017
GS-2015B-Q-501 data from August 1st, 2016 to January 31st, 2017
GS-2017B-Q-500 data from August 1st, 2017 to December 31st 2018
GS-2017B-Q-501 data from August 1st, 2017 to December 31st 2018
Letters of Intent for Campaign Science Proposals
Update: Titles, PIs, and PI contact information for the submitted letters of intent are available. We encourage the development of collaborative campaign programs that will yield significant scientific results and remind proposers that participation across the Gemini Partnership is a criterion by which proposals will be evaluated.
This page is also available as a pdf document.
GPI Campaign proposals are expected to embrace a large, scientifically compelling and statistically significant investigation in the chosen science area. While GPI's primary science goal is the detection and characterization of exoplanets, its high contrast capabilities will allow significant scientific advances in such areas as circumstellar disks, stellar evolution and mass transfer, fundamental stellar astrophysics including binaries, and Solar System objects. All areas are open to campaign science proposals. Collaboration of teams from across the Gemini partnership is encouraged, and partner participation is a criterion by which campaign proposals will be evaluated.
Gemini will select the scientifically compelling proposal or proposals for scheduling. We anticipate considering programs that request from 200 to 1200 queue hours of telescope time, but this does not strictly limit the amount of time that letters of intent may suggest.
Prospective GPI Campaign Projects should submit a Letter of Intent to the Gemini Deputy Director/Head of Science by January 20, 2011. Letters should include this information:
- Title of Project
- Principal Investigator with full name of institution and contact information (phone and email)
- Co-Investigators with full names of institutions
- Broad scientific goals of the program
- An estimate of the total amount of telescope time that will be requested and the number of semesters over which the project will run
- A brief justification for the required time, not to exceed three pages
The primary purpose of this Letter is to give the Gemini Science Committee an indication of the level of interest in GPI Campaign time so they can make a recommendation to the Board on the total time available for GPI Campaigns. The Letters of Intent will also inform the Gemini partners of the expected lien from GPI Campaign Projects on their usual allotment of Gemini time. Please send letters of intent to Gemini Deputy Director/Head of Science, Nancy Levenson, nlevenson at gemini.edu.
The Instrument
General information about GPI is available from the instruments section of the Gemini website (copied in a separate document), and current updates on GPI can be found at the external instrument site.
Policies for GPI Campaign Projects
This page is also available as a pdf document.
The GPI Campaign Projects represent a significant investment of resources by the Investigators on the projects, by the Gemini Observatory in executing the projects and by the Gemini partnership in granting the telescope time. The following are the expected policies that will govern GPI Campaign Projects.
- Prospective GPI Campaign Projects should submit a Letter of Intent to Gemini by January 20, 2011. Letters should include this information:
- Title of Project
- Principal Investigator with full name of institution and contact information (phone and email)
- Co-Investigators with full names of institutions
- Broad scientific goals of the program
- An estimate of the total amount of telescope time that will be requested and the number of semesters over which the project will run
- A brief justification for the required time, not to exceed three pages
The primary purpose of this Letter is to give the Gemini Science Committee an indication of the level of interest in GPI Campaign Time so they can make a recommendation to the Board on the total time available for GPI Campaign Proposals. The Letters of Intent will also inform the Gemini partners on the expected lien from GPI Campaign Projects on their usual allotment of Gemini time. Additional details about the Letters of Intent are described in a separate document.
- The time for GPI Campaign Science will be allocated off the top in an amount decided by the Gemini Board following a recommendation from the GSC. It is expected that all partners will contribute to the GPI campaign time in proportion to their partner share.
- GPI Campaign Projects are to be handled similar to normal proposals in terms of time requests. Each GPI Campaign Proposal will indicate the requested number of hours per semester. Campaign program PIs must be eligible for time on Gemini South. University of Hawaii does not have time at Gemini South at present, so they cannot apply for GPI Campaign Time through the UH host time, but they may apply through the US.
- A GPI Campaign TAC will assess proposals and make recommendations to the Gemini Director. The GSC will make recommendations on the size and makeup of the TAC following receipt of the Letters of Intent. The Letters will also allow the GSC to identify conflicts of interest when populating the TAC. The Campaign TAC will include representation from the International TAC. This TAC will be the basis for the GPI Campaign Working Group that will evaluate progress of the ongoing approved programs.
- Gemini will appoint a staff member to be the GPI Campaign Program Manager. This person will be responsible for the oversight of the successful GPI Campaign program(s) and will serve as the interface to Gemini for policy issues. Issues related to operation of the campaign programs will be handled the Head of Science Operations for Gemini South.
- Gemini will not provide a funding award to support GPI Campaign Science.
- Approved campaign targets and their observing modes will be made public. Observations using a substantially different mode or instrumental setup may be considered for target duplication in independent programs.
- The Call for GPI Campaign Proposals is expected to be issued on February 1, 2011, with an expected deadline of March 31, 2011, for receipt of proposals.
- GPI Campaign Proposals must include:
- a discussion of the primary scientific goals of the project;
- a description of the experimental design, including sample selection, use of GPI, scheduling requirements, calibration, etc.;
- a statement of the time requested by semester and by science ranking band;
- a description of data products compatible with the international virtual observatory to be delivered, and the timeline for their delivery;
- a management plan that describes staffing and resources available to complete the science program. The management plan must also describe:
- the expected contributions of each participant;
- data management procedures, including access to data within the team;
- who is responsible for submitting progress reports and final reports;
- the process for redirecting the research agenda as discoveries are made;
- the mechanism for routine communication among research team members.
Additional details about the Campaign Proposals are described in separate document.
- Each approved GPI Campaign Project will require a “Research Collaboration Agreement” signed by all members of the team before the campaign starts. This document needs to address the following questions:
- What are the scientific issues, goals, and anticipated outcomes or products of the collaboration?
- When is the project considered to be complete?
- What are the expected contributions of each participant?
- How and by whom will data be managed? How will access to data be managed? How will long-term storage and access to data after the project is complete be handled?
- Who will write any progress reports and final reports?
- How will the team decide about redirecting the research agenda as discoveries are made?
- What will be the mechanism for routine communications among members of the research team (to ensure that all appropriate members of the team are kept fully informed of relevant issues)?
- How will the team negotiate the development of new collaborations and spin-off projects, if any?
- How, and by whom, will personnel decisions be made? How and by whom will personnel be supervised?
- What will be the criteria and the process for assigning authorship and credit?
- What is the process for pursuing independent or novel results based on the campaign data?
- How will credit be attributed to each collaborator's institution for public presentations, abstracts, and written articles?
- How and by whom will public presentations be made?
- How and by whom will media inquiries be handled?
- When and how will intellectual property be handled?
- Should one of the principals of the research team move to another institution or leave the project, how will data, and authorship, and credit be handled?
- What is the procedure for adding new members to the research team?
While the SDSS is a much larger collaboration, it may be useful to look at examples of their various collaboration agreements
- Each successful GPI Campaign Project is to submit annual progress reports to the Gemini Director. These reports should contain (at a minimum) a summary of the observing time used thus far, comments on the quality of the data and whether the data quality is sufficient to meet the scientific goals of the program, a summary of the activities of each team member, the status of reduction of the data, and detailed plans for the next year of the project. With advice from the GPI Campaign Working Group, Gemini and the GSC will assess these reports to determine if continuing campaign observations are warranted.
Public Data Readme
GPI Public Data Early Release Readme
Contributors:
GPI first light observing team: Bruce Macintosh, James Graham, Stephen Goodsell, Les Saddlemyer, Dave Palmer, Jeff Chilcote, Andrew Cardwell, Jennifer Dunn, Ramon Galvez, Gaston Gausachs, Markus Hartung, Pascale Hibon, Patrick Ingraham, Marshall Perrin, Lisa Poyneer, Carlos Quiroz, Fredrik Rantakyro, Naru Sadakuni, Dmitry Savransky, Andrew Serio, Sandrine Thomas, Kent Wallace, Schuyler Wolff
GPI data analysis team: Marshall Perrin, Jerome Maire, Patrick Ingraham, Dmitry Savransky, Christian Marois, Rob De Rosa, Jeff Chilcote, Rene Doyon, Zack Draper, Quinn Konopacky, Franck Marchis, Max Millar-Blanchaer, Jennifer Patience, Laurent Pueyo, Abhi Rajan, Jean-Baptiste Ruffio, Sandrine Thomas, Jason Wang, Kim Ward-Duong, Schuyler Wolff
Description of Targets
The targets for this data release fall into five categories:
-
Photometric/Spectroscopic standards. Most of these were observed open loop (i.e. AO control off) and unblocked by the coronagraph to measure system throughput while avoiding saturation. Some targets were observed with and without the apodizers and Lyot stops to measure the relative throughput of the coronagraph masks. The targets are from the IRTF Spex spectral library (HD 51956, HIP 30979, HD 20619), plus the white dwarf companion to HD 8049 from Zurlo et al. 2013.
-
Astrometric Standards. Trapezium stars Theta1 Orionis A and B (compare with Close et al. 2013), and HD 1160 (compare with Nielsen et al. 2012).
-
Bright overhead test targets (but otherwise undistinguished stars). During the first run we tested the AO system and coronagraph on a series of targets chosen primarily for brightness and position in the sky. We include these as examples of GPI coronagraphy in a range of atmospheric conditions and observing bands, but caution that (a) these were early nights and instrument performance was very much in flux as operating parameters were adjusted, and (b) the seeing was relatively poor.
-
Stars with Known Planets and/or Disks. HD 95086 (H and K1 bands), Beta Pic (J band only), HD 10647 (J), HD 61005 (J).
-
Resolved Solar System Targets. Neptune (H band)
A subsequent data release(s) will add targets in polarimetry mode and in GPI’s non-redundant aperture masking (NRM) mode. The GPI team is still working to improve calibration of these modes and handling of some systematics before releasing these data.
Finally, other targets have been observed but remain proprietary to the GPI team for the time being, including Beta Pic (H, K1, K2 bands) and HR 8799 (K1 and K2 bands).
Important Cautionary Notes
The released FITS files represent the GPI instrument team’s best effort at calibrating and reducing these observations, but instrument calibration is necessarily a work in progress and incomplete. GPI is a highly complex instrument that we are still getting to know. Use your own experience and scientific judgement when analyzing and publishing data from GPI.
In particular, the stability over time of GPI’s absolute orientation with respect to the sky has not yet been characterized. Position angles should be considered uncertain to ~ 1 degree.
Every commissioning comes with surprises. For GPI these included:
-
More vibration than desired, due to the cryocoolers on the IFS. This manifests as tip-tilt and focus jitter in these data, and reduces contrast by ~ 0.3 mag for many targets. Instrument modifications in January and February 2014 are expected to mitigate this. Note also that contrast degradation is a function of angular separation.
-
Somewhat lower throughput was achieved than expected, with particularly sharp falloff beyond 2.2 microns in the K2 band. This is still being investigated. GPI’s design and optical coatings were optimized for performance at shorter wavelengths such as H band.
-
An artifact identified before commissioning—an optical ghost called the ‘seagull’ that can be seen in flat field or arc lamp images—is due to a caustic reflection inside the IFS of light from outside the field of view. A new baffle was installed in January 2014 to mitigate this.
-
The brightness ratios of the satellite spots relative to one another are variable at a level of up to a few tens of percent. This is believed to be due to an interference phenomenon between speckles and the diffracted spots. Quantitative models and calibrations are under development. Users should be cautious in assessing uncertainties when conducting photometry relative to satellite spots, and should not rely solely on any one single spot.
-
The lenslet (spaxel) pixel scale appears to be exactly as expected, 14.3±0.1 mas/lenslet. Distortion has not yet been characterized on sky; laboratory tests measured median distortion of 0.26 spaxels over the full field of view, and a correction based on these lab measurements is included with the data pipeline, which should reduce residual distortion to <0.04 spaxels.
-
Due to IFS internal flexure, the microspectra shift locations with respect to the detector, generally less than one pixel but with occasional larger shifts. Calibrations for this are still being improved. The wavelength calibration of the reduced data files should be considered uncertain by ~0.2% (~ 3 nm). Shifts will vary from image to image depending on changes in elevation.
Data Reduction Notes
We summarize here the steps by which the raw data were reduced for this data release. Readers should also consult the GPI data pipeline documentation for additional descriptions of the individual steps in processing. As with all outputs of the GPI data pipeline, detailed reduction history and all reduction parameters are saved in FITS headers, so consult those for full details.
The data were reduced with v1.0rc1 (release candidate 1) of the GPI data reduction pipeline using the following primitives:
-
Flag Quicklook
-
Load wavelength calibration
-
Subtract dark background
-
Destripe science image (a)
-
Interpolate bad pixels in 2D frame
-
Update spot shifts for flexure
-
Assemble spectral datacube
-
Divide by lenslet flat field
-
Interpolate wavelength axis
-
Correct distortion
-
Measure satellite spot locations (b)
-
Measure satellite spot peak fluxes (b)
(a) - Destriping only performed on J-band closed-loop data.
(b) - Satellite spots only measured in a subset of the closed-loop data.
Sky background observations were obtained for a subset of targets, offset by ~ 30 arcsec from the science objects. For this subset of observations, a sky cube was constructed through a median-combination of each reduced sky cube, which was then subtracted from each reduced science cube. For observations that lack contemporaneous sky data, no sky subtraction was performed in these reduced files.
Calibration files were selected either automatically or manually for the following primitives:
Load wavelength calibration -- automatic
Subtract dark background -- automatic
Interpolated bad pixels in 2D frame -- automatic
Divide by lenslet flat field -- manually (S20131212S0004_lensletflat_spec.fits)
Correct distortion -- manually (S20121210S0066-distor.fits)
The default recipe parameters were only changed in two instances; (1) when an offset was needed to align the wavecal solution with the spectra in the unprocessed 2D images, and (2) when the automatic satellite spot location algorithm failed due to low SNR on the satellite spots:
1 - Wavecal offset
For a subset of the reductions, the offset obtained from the lookup table in the ‘Update spot shifts for flexure’ primitive were not sufficient to fully correct for the flexure of the instrument. This problem manifests itself as a strong Moire pattern within each slice of the reduced data cube, which is discussed under ‘Reducing your science data’ here:
http://docs.planetimager.org/pipeline/usage/tutorial.html
For observations where the offsets obtained from the lookup table led to a poor reduction, GPItv was used to determine the correct offset to apply by visually aligning the spectra within the 2D image with the overplotted wavecal solution. This offset was then entered into the ‘manual_dx’ and ‘manual_dy’ parameters of the primitive, with the ‘method’ parameter changed to ‘manual’, and the data were re-reduced. As the expected change in the offset caused by instrument flexure as a function of target elevation was small for a given set of observations on a target (typically <0.2px), a single offset value pair was used for each sequence of a given target. This procedure was necessary for the following observations:
All Y-band
All J-band
H-band observations of Neptune
All K2-band
Improved automation for flexure compensation is under development for future versions of the data pipeline.
2 - Satellite spot finding
For a subset of closed-loop observations taken under poor seeing conditions, or for which the satellite spots are only marginally detected, the automatic spot-finding algorithm (‘Measure satellite spot locations’) fails during the reduction process. In this case, the data are initially reduced without the final two satellite spot primitives. The pixel position of the spots in the 15th frame were measured manually, and the data were re-reduced with the following modifications to the parameters in the ‘Measure satellite spot locations’ primitive:
reference_index = 15
loc_input = 1
x*, y* = [x, y pixel position of the corresponding satellite spot]
The next release of the data pipeline will include refinements to the automated spot-finding algorithm which will hopefully increase its success rate. However, images with very low SNR in the spot locations will almost always need to be reprocessed manually to locate the spots.
Using the Satellite Spots:
The measured satellite spot locations and fluxes are written to the extension header in each FITS file, along with the derived mean star locations (keywords SATSi_j for sat spot locations, SATFi_i for sat spot fluxes, where i gives the wavelength index and j in {0-3} indexes the four spots.) Keywords PSFCENTX and PSFCENTY give the star locations; Note that these are the mean locations across the spectral axis, but due to atmospheric differential refraction the star’s apparent position will generally vary with wavelength. (These data were all obtained prior to GPI’s atmospheric dispersion corrector being commissioned for use, so ADR is uncompensated). The wavelength dependent position may be computed from the SATSi_j keywords and used to align the wavelength channels.
The satellite spots can also be used for photometry relative to the central star. The satellite spot intrinsic brightness ratios have been measured in the lab for each apodizer (one per filter). See the file config/apodizer_spec.txt included with the data pipeline. Datacubes may be calibrated into physical flux units using the “Calibrate Photometric Flux” primitive in the data pipeline.