Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.0Assigned ID: 3110
----- Attempting Submission 1 (Fri Mar 25 02:32:03 GMT 2022) -----G160M requested SNR is less than 20.Therefore warnings flagged are not valid.For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.All FP-POS are selected for each setup per target allocated over multiple visits.
Updated Visit 11 with new cenwave.543351688----- Attempting Submission 1 (Wed Jul 13 14:48:54 GMT 2022) -----
----- Attempting Submission 2 (Wed Aug 23 15:52:55 GMT 2023) -----
----- Attempting Submission 3 (Mon May 06 19:29:51 GMT 2024) -----
----- Attempting Submission 4 (Fri Dec 20 10:31:19 GMT 2024) -----
----- Attempting Submission 5 (Mon Jan 27 14:27:13 GMT 2025) -----All FP-POS settings are selected for each setup per target, allocated over multiple visits.
Some warnings are for greater than 2400s integration in LP6 position.
We are satisfyling the FP-POS conditions while maximizing SNR.
Target 2 HB89-0906+015 is a quasar and doesn't have any proper motion. The error flag in the APT is redundant.Search for feedback signatures in massive blue galaxy halosThe quenching of star formation creates the red sequence of galaxies, which accounts for most of the stellar mass in the Universe today. Hubble/COS studies of mainstream galaxy populations show that the Circumgalactic Medium (CGM) has some connection to quenching, as red galaxies generally have less warm halo gas than their star-forming counterparts but still exhibit substantial cold gas. This is a major conundrum: why do massive red galaxies retain a significant mass of cold gas but do not use it to form stars? We propose a systematic absorption-line experiment to answer a very well-posed question: what happens in the CGM of galaxies that are soon to quench? We have selected a sample of 20 QSO/galaxy pairs that combines 12 new QSO sightlines and six archival QSOs, all within 250 kpc projected separation of extremely blue and massive (log M*/M_sun>11) galaxies that are, or are about to be, transformed into quiescent red-sequence galaxies. New COS observations will probe the multiphase CGM using the O VI line to trace the hot gas and lower ionization species (H I, O I, C II/III, Si II/III/IV) to identify the cooler material. Combined with ground-based spectroscopic and morphological information on these massive blue galaxies, the new data will show where massive blue galaxies fit into the evolutionary sequence of galaxies and their CGM: Will their halos be full of metal-enriched gas still fueling star formation, like mainstream L* galaxies? Or has their halo gas started to fade away, driving them toward the red sequence? Our sample will apply proven techniques to an important phase of galaxy evolution where the baryon cycle has not yet been explored.We will observe 12 UV-bright (16.9 < FUV < 18.95) QSOs with HST/COS G140L and G160M/G130M to study the extended circumgalactic medium around a set of massive blue galaxies. Each target requires between 2 and 8 orbits (with a combination of G140L and G130M/G160M), amounting to 56 orbits in total for the program.
S/N Requirements:
----------------------
For each target, we use the COS G140L grating as at 0.2 < zgal < 0.6, both the Lyman limit and Ly-alpha fall in the G140L wavelength coverage, providing us with measures of HI column densities over 16.5 < log N(H I) < 18.0 (via the Lyman break) and log N(H I) > 20 (via the Ly-alpha damping wings). The survey design requires us to reach SNR ~ 10-12 at ~1500 AA with G140L setup.
We will further use the G130M or G160M grating (depending on z) to target HI 1025, OVI 1031, 1037, CII 1036, CIII 977, OI 1039 lines at 15-20 km/s resolution, which will provide detailed component structures and relative kinematics of the multiphase CGM gas. Moreover, HI 1025 (Ly-beta) line will be optically thin for log N(H I) < 15.0 and will provide accurate HI column density estimate in that regime. Combined with G140L measurements, we will have accurate HI column density measure for the full sample. We require SNR ~ 8-10 at the observed wavelength of OVI 1031 line. These S/N ratios enable good absorption-line measurements down to observed- frame equivalent widths Wl ~ 50 - 80 mAA at 3sigma, depending on wavelength (OVI detection threshold log NOVI ~ 13.5).
Instrument Set-up:
------------------
Each target will be observed with G140L grating at a central wavelength of 1280 AA, to cover the Lyman Limit and Ly-a absorption in the rest frame of foreground galaxy.
In order to adequately model the absorption features and detect their component structure, we choose the highest spectral resolution of COS (G130M/G160M, depending on galaxy redshift) with different central wavelengths. In addition to detecting Ly-beta and OVI, other transitions we probe will include C III 977, CII 1036 , OI 1039, Ly-gamma etc.
Phase II Strategy:
-------------------------
Our coordinates are accurate to within 0.4" and are all point sources. We use a NUV ACQ/IMAGE target acquisition strategy which maximizes the science exposure times for these sources. To calculate acquisition exposure times using the ETC, we require a S/N of 20 in these NUV acquisition images and model the QSOs as FOS-based QSOs using their Galex FUV magnitudes.
For every target we are using G140L grating centered at 1280 AA. And for each target we use either G130M or G160M gratings with different cenwave settings. We generally split our observations of each target into 3 or 4 orbit visits. For targets that require more than 4 orbits, we break them up into 2, 3 or 4 orbit visits. All our targets are observed between 1 to 3 visits.
To maximize exposure time and reduce overhead, we generally allocate one or two FP-POS per orbit. We split the FP-POS settings across different orbits and visits to ensure that all the FP-POS are uniformly used. Only exception is if there are FP-POS restrictions for that cenwave setting (e.g. for G130M, cenwave= 1291 both segments). In general, we uniformly distribute all FP-POS settings across all visits between all grating and cenwave settings.
None of these QSOs will pose a bright limit threat to COS and we have no timing or orientation constraints. In general, the buffer times are quite long, and we set the buffer time in the exposure manually to be approximately 2 /3 times the buffer full time from the ETC calculations. In our final set-up, we achieve SNR of between 9 - 10 across 1400 - 1550 Angstroms for all of our targets, which is in generally line with the requirements we outlined in the science case of Phase 1.All the team members are highly experienced in observations, interpretation, and analysis of CGM science with both ground and space based observations.
Dr. Rongmon Bordoloi is an expert in studying CGM and galaxy-halo gas connections, and imaging+spectroscopic observations from both ground and space. He has been involved in more than ten publications using HST/COS observations, which led to several NASA press releases. Dr. Bordoloi will lead the program, with survey design, data analysis and science results. He will also manage contribution from the Co-Is.
Dr. Jason Tumlinson and Dr. Andrew J. Fox are experts on observations of the CGM with HST/COS, the instrument used in this proposal. Both Dr. Tumlinson and Dr. Fox, will contribute to the survey design, provide input on the analysis and interpretation of results and on reduction of HST/COS spectra.
Prof. J. Xavier Prochaska is an expert in CGM observations using both space and ground based instruments. Prof. Prochaska's institutional access to Lick/Keck observatories will be crucial in obtaining ground based optical follow-up of the northern galaxy targets in this proposal.
Prof. Robert A. Simcoe is an expert in CGM observations, specially at high redshifts. Prof. Simcoe's institutional access to Magellan telescope has been vital in obtaining ground based optical follow-up of the equatorial/southern galaxy targets in this proposal.
Prof. J. Christopher Howk and Dr. Nicolas Lehner are both experts on observations of the CGM with COS, the instrument used in this proposal. They are leading a survey to study the CGM of massive red galaxies, which will be provide a vital comparison sample for this project. Prof. Howk's institutional access to the LBT telescope will be vital in obtaining ground based observations of quasars and galaxies.
Dr. Joseph N. Burchett is an expert on CGM observations with HST/COS. He will contribute in survey design and ground based campaigns for galaxy spectroscopy.
Dr. Benjamin Oppenheimer is an expert in computational hydrodynamic simulations of galaxies and their gaseous environments. He specializes in understanding how the physical and evolutionary parameters of the IGM/CGM can be quantified through observational campaigns. He is an expert at interpreting COS UV data.
Dr. John M. O'Meara is highly experienced in using both space and ground based instruments. Dr. O'Meara will contribute to the interpretation of results, and reduction of ground based follow up observations. Dr. O'Meara also has institutional access to the Keck telescope which will be vital for the ground based optical follow-up campaign.
All the team members combined, have published more than hundred papers on the topic of CGM and galaxy-halo gas connection which have resulted in numerous NASA press releases (e.g., the recent Tumlinson et al. 2017 review on the CGM).Intergalactic Medium and the Circumgalactic MediumGalaxies6falsetruefalsefalsefalsefalseSUPPORTEDGALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000Galex_FUV = 18.95GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000Galex_FUV = 18.39GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000Galex_FUV = 16.91GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000Galex_FUV = 17.97GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000Galex_FUV = 18.66GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000Galex_FUV = 18.56GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000Galex_FUV = 18.13GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000Galex_FUV= 17.26GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000Galex_FUV = 17.79GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000Galex_FUV=17.83GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000Galex_FUV=17.69GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000Galex_FUV=17.98COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1533The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.First visit to do 3 orbits of G140L and 1 orbit of G130M.170003489100046.64920000000001(Tic-Visit
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