For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.0Assigned ID: 5125
----- Attempting Submission 1 (Sun Mar 24 18:49:17 GMT 2024) -----
HST Phase I Proposal 5125 successfully submitted.
Receipt: # 5125-1The error relates to noise considerations with the COS G160M mode, which has been taken into account in our ETC.COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.Fixed FP-POS to toggle between allowed lifetime positions of COS.-1678347331----- Attempting Submission 1 (Thu Aug 15 23:09:08 GMT 2024) -----
HST Phase II Proposal 17786 successfully submitted.
Receipt: # 17786-1
----- Attempting Submission 2 (Thu Aug 15 23:16:15 GMT 2024) -----
HST Phase II Proposal 17786 successfully submitted.
Receipt: # 17786-2
----- Attempting Submission 3 (Thu Oct 10 17:50:31 GMT 2024) -----
HST Phase II Proposal 17786 successfully submitted.
Receipt: # 17786-3
----- Attempting Submission 4 (Thu Oct 10 17:52:48 GMT 2024) -----Warnings are regarding the COS PSA for extended objects. The warning is not of concerns for our program: the ultimate science interest is an extended object, but the object in the COS aperture is effectively a point source (background galaxy).Tracing the beginnings, endings, and rarity of Blue Ring Nebulae to a rare stage in post-stellar merger evolutionWe catch stellar mergers in the act as luminous red novae (LRNe), peaking several orders of magnitude at optical wavelengths, then decaying exponentially and reddening. LRNe are incredibly difficult to study immediately afterwards. Outflows launched by a merger expand quickly and cool rapidly, forming obstructing dust and molecules that block our view just days-weeks afterwards. Even suspected ancient mergers, like CK Vul, are still embedded in dusty envelopes. We have no observational evidence for what happens to stars after they merge. What do systems look like after merging? What are the long-term ramifications of stellar mergers?
The Blue Ring Nebula (BRN) is a rare example of an outflow, produced by a thousands of years old stellar merger, that has virtually no obstructing dust in it, thus revealing the star that created it, TYC 2597-735-1 (TYC). We propose to use HST-COS G130M and G160M spectra to characterize the BRN by observing a fortuitously-positioned background galaxy to probe it using absorption line spectroscopy. Far-UV observations
are exclusively able to cover molecules, neutral, and ionized gas at a wide range of temperatures. Absorption line depths are sensitive to how much matter is in the sightline, so H2, HI, and residual gas in the BRN will stick out against the continuum source. The BRN is quickly expanding towards us, so lines traditionally washed out by airglow or interstellar absorption (e.g., HI) will be velocity-shifted away from these contaminants. This powerful technique will uncover the composition, density, temperature, and motions of the BRN gas, answering key points about its origins, its lifetime, and the number of BRNs we might see.Program Overview: This Cycle 32 GO program requests 22 orbits in total, split between COS G130M/1291 and G160M/1533 (11 orbits in each mode), to observe the properties of neutral hydrogen (HI, H2) and reveal hidden residual species in the Blue Ring Nebula (BRN) using absorption line spectroscopy:
- COS G130M (1291) accesses both HI and cool/warm phases of H2 through the BRN;
- COS G160M (1533) accesses the warm/non-thermal populations of H2$ in the nebula.
Both G130M and G160M modes access many strong features of neutral and ionic C, N, Si, O, He, and other species that may be too sparse to show up in emission. These COS grating positions provide sufficient far-UV spectral coverage of HI-LyA in absorption (which is expected to be blue-shifted by >= 400 km/s from line center, avoiding geo-coronal emission and interstellar HI absorption, which is estimated to be ~10E20 cm-2, based on IRSA extinction maps) and numerous absorption bands of H2. Access to H2 absorption signatures depends strongly on the thermal temperature and non-thermal populations of the molecules in the BRN (H2 Lyman-Werner electronic transitions: 1120 - 1700 \AA). This information is currently unknown, so even a non-detection at our requested signal-to-noise (SN) places important constraints on the properties of the remaining molecular reservoir of the BRN and its properties. The COS G130M and G160M modes are sensitive enough to probe all the above features within our observing plan while achieving spectral resolutions (R ~ 17,000) necessary to sufficiently model the kinematics, density, and temperature of the nebular gas.
The galaxy SDSSCGB 73656.1 is the only FUV-bright source found behind the BRN, with a measured FUV flux = 19.6 mag (GALEX), making this absorption line study possible. SDSSCGB 73656.1 is redshifted slightly (z=0.0818), and its UV continuum is expected to peak in the FUV range covered by our COS observations. Any galactic absorption features will be redshifted from their rest frame wavelengths and treated as contamination in our analysis. We will avoid spectral regions around suspected contamination lines.
At the Galactic latitude of the BRN (+35 degrees), the HST viewing window is expected to be 55 minutes. Assuming 2550 seconds of science exposure per orbit, this allows for 740 seconds of slew and settle time. Each observing mode allows adequate time for guide star acquisition (using ACQ/SEARCH PSA), instrument acquisition, a single peak up, and a buffer dump prior to the science exposure. There are a number of guide stars choices in the field of SDSSCGB 73656.1 that prove adequate for acquisition (e.g., TYC 2597-735-1: V = 11.1 mag).
COS Instrument Safety: We do not expect any bright features to show up in either G130M or G160M. The BRN itself, in emission, is very faint (F(FUV) ~ 8E-18 ergs/cm2/s/arcsec2). The galaxy continuum is expected to be the brightest astrophysical source, and will not peak more than ~ 1E-13 ergs/cm2/s. This results in ~$0.002 counts/second in the brightest pixel. Geocoronal LyA will be the brightest feature in G130M, at 0.095 counts/second in the brightest pixel (according to the COS ETC). In G160M, the brightest pixel will be the continuum of SDSSCGB 73656.1 at the most efficient part of the spectrum, which results in a max count rate of 2.260e-04 counts/second in the brightest pixel (verified with COS ETC). Since the count rate limit of the COS FUV XDL detector is ~ 0.67 counts/second/pixel for both modes, all fluxes are well within COS observing capabilities.Dr. Keri Hoadley (PI) is an expert in molecular fluorescence and UV spectroscopy. She has both built a high resolution far-UV spectrograph, which has flown aboard several sounding rocket missions (Hoadley et al. 2014, 2016, 2020), and written several papers on the data reduction and analysis of warm molecular regions in planet forming disks using HST-COS spectra (Hoadley et al. 2015, 2017, 2020a). She led the discovery paper of the Blue Ring Nebula (Hoadley et al., 2020b). Dr. Hoadley will work with a graduate student at the University of Iowa to fit SDSS models of the galactic background, extrapolated into the UV bandpass, to separate the galactic background source from the BRN spectral features, as described in the proposal.
Dr. Chris Martin was a key member and PI of the GALEX science team responsible for the discovery of the Blue Ring Nebula. He is also an expert in LyA radiative transfer and wrote the discovery paper of H2 fluorescence in the diffuse ISM.
Dr. Nicole Arulanantham specializes in UV molecular absorption and emission line characterization and modeling. She will use her expertise in H2 fluorescence modeling to help guide modeling efforts of observe H2 absorption features, weigh in on interpretation of the spectra, and help explore statistical approaches to setting upper limits to molecular densities and populations, in the event that no H2 absorption is detected in the BRN
sightline. Dr. Kevin France is an expert in UV spectroscopy, in particular H2 fluorescence. With Dr. Hoadley, he will help interpret the H2 absorption signatures we measure from the BRN and diagnose its physical state. He will provide guidance on residual gas tracers (e.g., other neutral and ionic species besides hydrogen).
Drs. Moritz Guenther and Christian Schneider are experts in both UV and X-ray spectroscopic diagnostics in pre-main sequence accretion disks.and astrophysical shocks and jets. Dr. Casey DeRoo is experiences in high energy astrophysics and X-ray data analysis. They all bring extensive knowledge of accretion and shock interpretations, as well as analysis techniques and insight that compliment the scope of this program.
Drs. Brian Metzger and Dr. Ken Shen provide analytic and theoretical perspective to this program, both having been key to unraveling the origins of the Blue Ring Nebula and its relationship to TYC 2597-735-1. Both intuitively tie observational evidence to theory and will provide this perspective for future literature published using these novel datasets.Stellar Physics and Stellar TypesStellar Populations and the Interstellar Medium6falsetruefalsefalsefalsefalseSUPPORTEDGALAXYUNDESIGNATEDYESThis object was generated by the targetselector and retrieved from the SIMBAD database.WISEA-J164835.42+350939.0GALEXASC-J164835.47+350938.8J2000J2000GALEX FUV (AB): 19.6 +/-0.05, GALEX NUV (AB): 19.6 +/- 0.03, u(AB): 19.180 +/- 0.075, g(AB): 18.024 +/- 0.010, r(AB) 17.601 +/- 0.010, E(B-V) = 0.016COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1533/System/Volumes/Data/solaris/user1/crodriguez/work/hst/OP-cache/17786-v01.xmlThe scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Orbits 1-31743703513000246.61100213248199(Tic-Visit
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