0Assigned ID: 723
----- Attempting Submission 1 (Fri Mar 06 19:54:57 GMT 2020) -----
HST Phase I Proposal 723 successfully submitted.
Receipt: # 723-1
----- Attempting Submission 2 (Sat Mar 07 00:24:39 GMT 2020) -----The BOT reports 7 exposures with a health/safety object. However, those objects seem to be the targets themselves, because they have the same V-band magnitude as the targets.
I used the ETC to verify that the brightness limits were never reached. The highest count rate I encountered was around 127000.
I used the UV flux at the line of interest (1350A for E140H and 2325A for E230H) obtained (by eye) from an IUE spectrum to normalize the Kurucz model spectrum for each target.
To fill the orbits, I used the Auto-Adjust feature in the Orbit Planner. This automatically splits the unused orbit time equally over the exposures (if more than 1 exposure in the orbit).
I am not sure if there is maybe a better strategy to fill the orbits, e.g. by increasing the exposure times differently for different exposures, to maximize the SNR in both exposures.
Added duplicate of visit 7 as visit 18887010483----- Attempting Submission 1 (Tue Jun 30 15:35:34 GMT 2020) -----
----- Attempting Submission 2 (Thu Mar 04 22:12:10 GMT 2021) -----Linking dust extinction properties to depletion in the Milky WayWith this proposal we aim to investigate the relation between dust grain evolution, dust composition, dust extinction properties and environment in the Milky Way. To enable this, we need to expand the sample of depletion measurements, in particular to increase the number of sightlines with C and Si measurements, the two principal components of dust grains. We propose STIS spectroscopic observations towards 17 stars in a total of 31 orbits. These data (in combination with the available archival data) will allow us to study dust properties in a wide range of environments (from dense to diffuse gas clouds), and help us understand which mechanisms play a role in dust evolution in the Milky Way.We will observe 17 stars using the STIS Echelle spectrograph with the E230H/c2263 grating (to measure C, Si and Fe depletions). In addition, 12 of these stars need observations with the E140H/i1307 grating (to measure Mg and O depletions). High resolution UV spectra are needed to measure element column densities from absorption lines. The column density of a certain element is directly linked to the optical depth of its corresponding absorption line, which can be derived by comparing the measured line intensity to the continuum intensity (Sembach & Savage, 1992). In order to measure the optical depth of a certain line, we need a sufficiently high SNR around that line. From the results presented in Jenkins (2009), we can roughly predict the column density of a certain element in a given sightline, using the hydrogen column density (N(H)) of that sightline, in combination with the Milky Way reference abundance and an estimate for the depletion of that element. The predicted column density can in turn be used to calculate the equivalent width of the absorption line of interest (using eq. 1. from Morton (2003)). Subsequently, the requested SNR to obtain a 4 sigma detection of this line can be estimated (based on eq. 1 in Tumlinson et al. (2002)). From this, we found that sightlines with log[N(H)] >~ 21.45 require a reasonable SNR <~ 65 to detect the weakest absorption line (CII line at 2325A). The actual required SNR to detect the CII line for every target depends on the hydrogen column density (N(H)) towards that target, and is lower if the density is higher. This determines the required SNR for the E230H observations, as the SiII line is somewhat stronger and the FeII line is much stronger than the CII line. For the E140H observations, all targets are bright enough to be able to detect the MgII and OI lines without any restrictions on the SNR. For these observations, we used a default SNR of 20 for all targets. The exposure time calculator for STIS predicts total exposure times between 400 and 5700 seconds per star.
We verified that the brightness limit for the MAMA detectors was never reached. We are confident about the count rate estimates of the ETC, as we used the UV flux obtained from an IUE spectrum (in the wavelength region of the grating) to normalize the Kurucz model spectrum for each target.
Description of possible implications of reduced-gyro operations:
Specifying a Gyro Mode of 1 for the visits in this program, and re-running the Orbit and Visit Planner, learned that reduced-gyro operations significantly reduce the visit schedulability for all visits. However, all visits are still schedulable. In case the total available exposure time in an orbit reduces, the SNR of the spectra would decrease, possibly resulting in non-detected absorption lines.The PI and both co-I's are experts in the study of interstellar dust. M. Decleir and K. Gordon are experts in studying the UV extinction and attenuation properties in the Milky Way and in nearby galaxies. K. Gordon is the PI or co-I of a number of HST programs to measure the UV dust extinction and HI column densities in the Milky Way and other Local Group galaxies. J. Roman-Duval is an expert on depletion measurements and is the PI of METAL and METAL-Z, two HST programs to investigate the metal abundances and depletions in the LMC and other low metallicity galaxies. She is an expert on analyzing STIS spectra and measuring gas column densities from absorption lines in these spectra.Stellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARMAIN SEQUENCE ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000STAREMISSION LINE STARMAIN SEQUENCE ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARMAIN SEQUENCE ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARALGOL SYSTEMB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARSUPERGIANT ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARB0-B2 III-INOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARSUPERGIANT ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARGIANT ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARGIANT ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARGIANT ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARSUPERGIANT ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARGIANT OMAIN SEQUENCE ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARB3-B5 V-IVEMISSION LINE STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARB3-B5 III-INOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARB0-B2 V-IVHERBIG AE/BENOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/FUV-MAMASpectroscopicNoNoE140H1307STIS/NUV-MAMASpectroscopicNoNoE230H2263The scheduling data was generated by CASM 29.0.CASM was run in Phase II mode.STIS observations of HD216898(Tic-Visit
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