0Assigned ID: 719
----- Attempting Submission 1 (Fri Apr 07 18:36:18 GMT 2017) -----
HST Phase I Proposal 719 (fireworks.apt) successfully submitted.
Receipt: # 719-1
----- Attempting Submission 2 (Fri Apr 07 20:37:34 GMT 2017) -----
HST Phase I Proposal 719 (fireworks.apt) successfully submitted.
Receipt: # 719-2
----- Attempting Submission 3 (Fri Apr 07 20:39:22 GMT 2017) -----
HST Phase I Proposal 719 (fireworks.apt) successfully submitted.
Receipt: # 719-3For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.The phase II has been modified following the response from the TTRB.
Only one target and one grating are now included.
The total exposure time has been split into two visits to improve schedulability.
11/03/17: Co-I James resubmitting on behalf of PI Belfiore:
Observing strategy has been revised: the four orbits within the two visits now alternate between FPPOS=3 and 4.
(Previous version had all FPPOS=3 in one visit, then FPPOS=4 in second visit). This allows for more exposure time on target and improved removal of fixed-pattern noise.-454476364----- Attempting Submission 1 (Thu Jul 13 12:28:04 GMT 2017) -----
HST Phase II Proposal 15125 (APT_PHASE_2.apt) successfully submitted.
Receipt: # 15125-1
----- Attempting Submission 2 (Wed Jul 19 14:44:49 GMT 2017) -----
HST Phase II Proposal 15125 (APT_PHASE_3.apt) successfully submitted.
Receipt: # 15125-2
----- Attempting Submission 3 (Sun Jul 30 22:34:19 GMT 2017) -----
----- Attempting Submission 4 (Fri Nov 03 15:37:14 GMT 2017) -----All the available FP-POS for G130M 1291 have been used. The other FP-POS are currently not offered.
Our science goals can be achieved with te current observing strategy (PSA COS spectroscopy of extended targets)Galactic fireworks: detecting young stars formed in galactic outflowsRecent observations have revealed massive galactic outflows of molecular gas, which may have the physical conditions required to form stars. Since outflows are complex, turbulent, multi-phase media, it has so far been challenging to conclusively identify star formation taking place in the flow via classical diagnostics. By exploiting high resolution, high sensitivity, broad band spectroscopy we have recently found evidence for star formation taking place in the fast galactic outflow of a nearby LIRG. We propose to obtain COS observations with two apertures sampling the outflow of this galaxy with the following goals: (1) obtain a direct detection of the hot, young stars formed in the outflow, which are expected to have the same velocity as the outflowing gas; (2) detect and measure the velocity of the young stars formed in the outer part of the outflow, where, according to models, they should form with velocities higher than the escape velocity; (3) determine the properties of the stars formed in the outflow, in particular their average temperature and metallicity; (4) measure the column density and metallicity of the outflowing gas, and thus constrain the amount of gas in the outflow and, therefore, the efficiency of star formation in this environment.We will observe IRAS2318-59 with an aparture centered on the brightest UV region associated with the southern nucleus (and sampling the inner region of the outflow).
We aim at obtaining very high quality spectra, similar or better than those obtained in James et al. (2014), which will enable: (1) a detailed analysis of the velocity profiles and velocity shift of the stellar and ISM absorption features; we plan to compare stellar and ISM kinematics both with each other and with the optical nebular emission and absorption lines tracing the outflow and stellar optical features; (2) disentangle the spectral features associated with the galaxy from the telluric absorption and emission features.
In order to achieve these goals we employ an observing strategy similar to James et al. (2014). We will adopt the G130M medium resolution grating (central wavelength at 1291), which covers the CIII 1176 and OIV 1342 young stellar features (in the rest-frame of the galaxy). The medium resolution grating is selected in order to accurately determine the gas kinematics and enable decomposition of line profiles. Given that some of the UV emission is extended on scales of ~1", this will result in to a degradation of the spectral resolution; however, thanks the medium resolution gratings, even with this degradation, the spectral resolution for this component will be still good enough (~60 km/s) to clearly associate the stellar kinematics with the outflow (velocity 300-500 km/s) or with the host galaxy. Also, the medium resolution grating ensures that the spectral features of interest are not blended with MW or telluric lines. The required setting will also enable us to observe numerous ISM lines from various elements in different ionization species and determine their column densities with uncertainties ~0.1 dex through a multi-component fitting technique. We will use the OI 1302 line to determine metallicity. If the line is saturated, we will instead use the SII triplet (1250, 1253, 1259).
Based on the ACS F140LP image of the galaxy, the proposed COS aperture has flux F(1500A)~6e-16 erg/s/cm2/AA. In order to perform the detailed analysis discussed above, to disentangle the kinematics of stellar populations with different ages we need to achieve a S/N ~ 15 per spectral resolution element. For the S/N calculation we take as reference wavelengths 1228 AA (which is the observed wavelength of CIII 1176). By using the ETC (with an O9-like spectrum normalized to the fluxes reported above), assuming a point source, the required S/N implies an exposure of 24ks.
We use standard peak-up target acquisition (TA) in NUV imaging mode exploiting the bright central UV clump in the proposed aperture.Galaxies and the IGM6falsetruefalsefalsefalsefalseSUPPORTEDGALAXYWINDYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1600/private/var/folders/ws/qrf1y4y905ngs2pwd3p701x80004q8/T/OPVisit10101059105581188.xmlThe scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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