0Assigned ID: 78
----- Attempting Submission 1 (Mon Mar 02 16:40:41 GMT 2020) -----The number of orbits used exceeds the number allocatedWhen I ran BOT, I see different numbers under "safe"; I don't know what they mean.
Please let me know if you see any issues and ifI need to do anything else.
Thank you for your help everybody!
updated with repeat for visit 4 by PC Wilson Skipper-1221408942----- Attempting Submission 1 (Tue Jun 23 15:48:34 GMT 2020) -----
----- Attempting Submission 2 (Fri Mar 19 19:54:12 GMT 2021) -----This is for a repeat submission, no need to run it againWhat governs the physics of the warm-hot circumgalactic medium?The properties of the circumgalactic medium (CGM) are governed by the
details of galaxy formation, evolution and feedback. The high
ionization lines of OVI are the most effective probes of the
warm-hot CGM of L* galaxies, because the ionization fraction of OVI
peaks at the virial temperature of these galaxies. An important
observational result in this field was published in Science; it showed
that the prevalence and strength of the OVI lines depend on the specific
star-formation rate (sSFR) of galaxies. However, there is a clear
correlation between sSFR and stellar mass in the observed sample, so the
governing parameter may be mass instead. Theoretical simulations are
also providing conflicting results, therefore new observations are
needed to inform the theory. We propose to probe the CGM of L* galaxies
at a range of sSFR, but at fixed mass. We will thus determine whether
mass or sSFR is the driving factor of CGM properties, or there is
additional physics. This will be a major step forward in our
understanding of the physics of gas inflows and outflows, star-formation
and feedback, and their relation to halo mass. This small program will
greatly enhance the scientific return on previous investments of
hundreds of orbits by clearly distinguishing between the possible
scenarios.We will observe all our targets with COS/FUV G130M.
Our main goal is to detect OVI 1032,1038 absorption doublet at the redshifts of intervening galxies. The G130M central wavelength has been determined accordingly. We will use recommended parameters FLASH=YES, and use the allowed Cycle 28 values for FP-POS. As recommended, we have split our total number of orbits per target into multiple visits of at most 3 orbits each.
Target acquision: From SIMBAD, we found precise coordinates of our targets. As per SIMBAD, the coordinate uncertainties are of the order of 0.1mas for all targets. Therefore will only use ACQ/IMAGE with NUV/MIRRORB
Target 1: 2MASSI-J1356327+210352:
The observed wavelength of OVI1032 is 1101.945A. Therefore we choose central wavelength=1222. We will use FP-POS=1, followed by FP-POS=2, followed by FP-POS=3 in visit 1. In visit 2 we will use FP-POS= 2, followed by FP-POS=3, followed by FP-POS=4. For visit 3 we will use FP-POS= 1, followed by FP-POS=3, followed by FP-POS=4. And for visit 4 we will use FP-POS= 1, followed by FP-POS=2.
Target2: VV2006-J003340.2-005525.
The observed wavelength of OVI1032 is 1213.4481A. Therefore we choose central wavelength=1291. In visit 1 we will use FP-POS=3, 3, and 4 in the three orbits and will use FP-POS=3, 4, and 4 in the three orbits in visit 2.
Target3: SBSG-0839+541.
The observed wavelength of OVI1032 is 1118.5107A. Therefore we choose central wavelength=1222. In visit 1, we will use FP-POS=1, followed by orbit 2 split in FP-POS=1, and =2, followed by orbit 3 with FP-POS=2. In visit 2, we will use FP-POS=3, followed by orbit 2 split in FP-POS=3 and FP-POS=4, followed by orbit 3 with FP-POS=4.
Target4: VV2006-J103440.9+443104
The observed wavelength of OVI1032 is 1262.1173A. Therefore we choose central wavelength=1291. We will use FP-POS=3 in orbit 1 and FP-POS=4 in orbit 2.
Target5: 2MASX-J08045271+2120504
The observed wavelength of OVI1032 is 1158.73398A. Therefore we choose central wavelength=1291. Both FP-POS=3 and FP-POS=4 are used in orbit 1.PI: Smita Mathur. Prof. Mathur is an expert on the
circumgalactic medium of galaxies, with several papers written on the
subject. She is also an expert on absorption-line spectroscopy,
particularly high ionization lines, and has experience with
spectroscopic data from HST. She has also obtained HST spectra as a PI
and as a co-I.
Co-I: Varsha Kulkarni. Prof. Kulkarni is an expert on the circumgalactic
medium and quasar absorption-line spectroscopy. She has successfully led
and completed several HST programs related to these topics. She and her
collaborators have published several papers making use of these HST
programs that used STIS, COS, NICMOS, WFC3.
Co-I: Yair Krongold. Prof. Krongold is an expert on
warm-hot plasma and absorption-line spectroscopy. He has written several
papers on the subject and he has also been successful in obtaining HST
data.
Co-I: Fabrizio Nicastro. Dr. Nicastro is also an expert on
warm-hot plasma and absorption-line spectroscopy. He has written several
papers on the subject using X-ray data and UV data from HST.
Co-I: Anjali Gupta. Prof. Gupta is an expert on the
circumgalacitc medium of galaxies, with several papers written on the
subject.
Co-I: Suraj Poudel. Mr. Poudel is a graduate student at
the University of South Carolina. He helped with culling the proposal sample.
Co-I: Arjun Karki. Mr. Karki is a graduate student
at the University of South Carolina. He helped with culling the proposal
sample.
Collectively, our team has authored many papers on the topics of the
circumgalactic medium and quasar absorption systems. We have been
successful in obtaining HST time and have written papers based on those
data. We are thus well-qualified to carry out the proposed project.Intergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV mag=17.38; NUV mag=17.25GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV mag=19.2294; NUV mag.=17.95GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV mag=17.73; NUV mag=17.76GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV mag=18.05; NUV mag=17.5394GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUNV mag=17.08; NUV mag=16.86COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291/System/Volumes/Data/solaris/user1/wskipper/OP-cache/16288-v01.xmlThe scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.1623662944000121.43530423447561(Tic-Visit
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