0Assigned ID: 613
----- Attempting Submission 1 (Fri Apr 07 16:17:27 GMT 2017) -----0----- Attempting Submission 1 (Mon Jul 10 20:51:53 GMT 2017) -----
----- Attempting Submission 2 (Wed Dec 12 18:02:25 GMT 2018) -----Probing CO-dark Gas within the Planck Galactic Cold ClumpsThe Planck Catalogue of Galactic Cold Clumps (PGCC) has identified the coldest regions of interstellar dust across the entire sky based on submillimeter emission. These sources range from relatively diffuse cold clouds to pre-stellar cores embedded in giant molecular clouds. In recent years, theoretical and observational evidence has shown that there exists a component of the cold molecular ISM that is "CO-dark" - that is, it contains very little carbon monoxide, the most common tracer of molecular hydrogen, and thus is hidden and unaccounted for in our measurements of the molecular content of the ISM. The PGCC represents an excellent test bed to probe for this CO-dark gas. To do so, we can use the high-resolution UV absorption line capabilities of the STIS instrument to probe for CO at higher sensitivities than CO emission line surveys. Furthermore, we can independently measure both the molecular hydrogen and total hydrogen content, which have been shown to correlate well with Cl I and O I absorption, respectively. As part of a previous archival survey, we identified existing STIS sightlines in the sky vicinity of PGCC objects, and found that a surprisingly small number of these sightlines displayed strong CO absorption. This general lack of CO absorption directly indicates the presence of CO-dark gas near these cold dust emission sources. However, our archival study found no high-resolution far-UV STIS spectra of any stars that lie directly behind a PGCC source. We now propose to observe seven sightlines that probe the central cores of these regions, allowing us to better characterize the prevalence and nature of CO-dark gas in these sources.We propose to obtain high-resolution (R ~ 110,000) STIS observations of selected inter- stellar UV absorption lines that were chosen based on their close vicinity on the sky to cold, dusty environments detected by Planck. Furthermore, we only selected sightlines that are clearly behind these regions, as determined by comparing Gaia parallax measurements for the stars to Planck distance estimates for the PGCC sources. We can address all of our stated scientific goals with the E140H echelle grating centered on 1343 A (covering the wavelength interval 1242-1444 A), and using the 0.2x0.2'' slit (except for the case of HD 217943, whose UV flux requires the use of 31x0.05NDB neutral density filter to avoid the MAMA bright limits). This setup will simultaneously capture the O I line at 1355.60 Angstroms, the Cl I lines at 1347.24, 1373.11, 1379.53, 1389.69 Angstroms, and the C I multiplets near 1277, 1280, 1329 Angstroms. It will also capture eight bands of molecular CO absorption between 1263 and 1419 Angstroms. We aim to achieve a spectral sensitivity of S/N ~ 20 for the Cl I line near the center of the bandpass.Stellar Physics6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARB0-B2 V-IVPULSATING VARIABLENOCoordinates, PMs, parallax and magnitude (and their associated errors) taken from the SIMBAD Database, when available. Listed as pulsating variable - analysis of Hipparcos light curve shows variability of order 0.02 mag (Dubath et al 2011).HR8777HIP113853J2000J2000STARB6-B9.5 V-IVBENOCoordinates, PMs, parallax and magnitude (and their associated errors) taken from the SIMBAD Database, when available. V magnitude error taken from Tycho-2 VT and BT magnitudesHIP80126J2000J2000STARB6-B9.5 III-IEMISSION LINE STARNOCoordinates, PMs, parallax and magnitude (and their associated errors) taken from the SIMBAD Database, when available. Error in V magnitude determined from Tycho-2 VT and BT magnitudes.HIP3932J2000J2000STARB3-B5 V-IVNOCoordinates, PMs, parallax and magnitude (and their associated errors) taken from the SIMBAD Database, when available.HIP53024J2000J2000STARB0-B2 V-IVBENOCoordinates, PMs, parallax and magnitude (and their associated errors) taken from the SIMBAD Database, when available. Error in V magnitude determined from Tycho-2 VT and BT magnitudes.HIP115224J2000J2000STARB6-B9.5 V-IVNOCoordinates, PMs, parallax and magnitude (and their associated errors) taken from the SIMBAD Database, when available.J2000J2000STARB6-B9.5 V-IVEMISSION LINE STARNOCoordinates, PMs, and parallax (and their associated errors) taken from the SIMBAD Database. V magnitude and its associated error determined from Tycho-2 VT and BT magnitudes.J2000J2000STIS/FUV-MAMASpectroscopicNoNoE140H1343STIS/FUV-MAMASpectroscopicNoNoE140H1343STIS/FUV-MAMASpectroscopicNoNoE140H1343STIS/FUV-MAMASpectroscopicNoNoE140H1343STIS/FUV-MAMASpectroscopicNoNoE140H1343STIS/FUV-MAMASpectroscopicNoNoE140H1343STIS/FUV-MAMASpectroscopicNoNoE140H1343The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.154347078600088.42073599440658(Tic-Visit
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