0Assigned ID: 929
----- Attempting Submission 1 (Fri Apr 10 22:18:47 GMT 2015) -----
HST Phase I Proposal 929 (HeII-PhaseI.apt) successfully submitted.
Receipt: # 929-1If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
ORBITAL VISIBILITY OVERRUN
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.I have updated acquisition exposure times for visits 1, 3, 6, 7, 9 & 10. This time assuming point-sources
throughout.
Previous (Feb 2016) comment:
Updated Phase II with corrected acquisition exposure for Visit 2 (1427-52996-221)
Previous (Dec 2015) comment:
This is an updated version of my phase II proposal with limitations on orientation for M77 (1070-52591-072).
I have included comments on the expected flux in the secondary aperture reported by the BOT tol.
Previous comment:
There were a number of BOT warnings for the objects. I have entered comments on this where relevant on the target page. It appears that all
are due to the BOT thinking that the object is a star when it is actually a galaxy.-285213813----- Attempting Submission 1 (Thu Jul 23 00:04:58 GMT 2015) -----
----- Attempting Submission 2 (Thu Dec 17 17:35:05 GMT 2015) -----
----- Attempting Submission 3 (Thu Feb 04 22:00:19 GMT 2016) -----
HST Phase II Proposal 14120 (HeII-PhaseII-adjusted-angle-fixed-visit2.apt) successfully submitted.
Receipt: # 14120-3
----- Attempting Submission 4 (Tue Apr 12 22:43:45 GMT 2016) -----There are warnings about the accuracy of target coordinates. These are in all cases known to better than 0.4" from SDSS data
There are also warnings about COS FUV PSA science exposures and their special calibration limitations. This is noted and in most
will be mitigated because the relevant UV emitting region is expected to be compact.He II emission as a tracer of ultra-low metallicity and massive star evolutionThe He II 1640 emission line is arguably the primary probe for detecting ultra-low metallicity star formation in the high redshift Universe but even at z~0 our understanding of it is woefully incomplete. Since the first signs of Population III star formation at high-z is even likely to be seen intermixed with more metal rich star formation, we need a solid understanding of the massive stellar population responsible for the excitation of He II at non-zero metallicity but this is currently lacking.
The main reason we do not fully understand the physics behind narrow-line He II emission at low metallicity is that we do not have any direct observational probes of the massive stars responsible for the ionizing radiation. Until we understand this, a significant uncertainty will remain in any interpretation of nebular He II 1640 at high redshift.
Here we propose to use COS to carry out the first systematic study of the massive stellar content in galaxies selected to have He II in emission. With this we will a) study in detail the population of massive stars responsible for exciting both narrow and broad He II, b) rigorously test recent claims for significant pockets of ultra-low metallicity star forming gas at 2<z<7 galaxies based on detecting narrow He II 1640 emission in deep spectroscopy.
This survey has only now become possible because we have carried out a systematic search for He II 4686 emitting galaxies at z~0. This allows us to accurately predict He II 1640 fluxes and therefore optimally design a COS observing program for these sources. A survey based on targeting UV bright galaxies/star forming regions would not be able to tackle these questions.The G160M grating with a central wavelength of 1589A is well suited
for observing He II 1640 and allows us to detect the majority of the diagnostic UV lines, in the range from 1400A to 1720.
To ensure optimal exposure time choices we estimate He II 1640 fluxes from the known He II 4686 fluxes, accounting for
dust attenuation using the observed Balmer decrement (Ha/Hb) and using an intrinsic
F_{1640}/F_{4686}=10 (e.g. Crowther & Hadfield 2006). We conservatively assume that the He II emitting region is uniform over
the aperture and use the resulting flux per unit area to estimate the exposure time needed with COS to reach an integrated S/N in
He II 1640 of 20. Since the equivalent width of He II 1640 is not expected to exceed 2-3A in these
galaxies (e.g. Brinchmann, Pettini & Charlot 2008), this will also suffice to detect the continuum in these galaxies with a good S/N (>7 per
resolution element in all cases).UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE12falsetruefalsefalsefalsefalseSUPPORTEDGALAXYSTARBURSTYESThe target fails BOT for the NUV acquisition. The object is however a galaxy and not a star and is extended. I do not have an HST image of the object but it is extended in SDSS u-band images thus I would argue it is safe.CGCG-007-025J2000J2000GALEX FUV=16.87 NUV=16.64 F(1640)=4.8E-15erg/s/cm^2GALAXYSTARBURSTYESThe object fails BOT. There is existing HST imaging in F336W which clearly resolves the object and the assumption of this being a point source for BOT calculations is clearly incorrect.J2000J2000FUV=16.67 NUV=16.55 F(1640)=6.8E-15erg/s/cm^2GALAXYSTARBURSTYESThe object fails BOT but is a clearly resolved galaxy.MRK1486J2000J2000FUV=16.73 NUV=16.78 F(1640)=2.7E-15erg/s/cm^2GALAXYSTARBURSTYESJ2000J2000FUV=17.99 NUV=17.81 F(1640)=4.8E-15erg/s/cm^2GALAXYSTAR FORMING REGIONSTARBURSTYESThere is a BOT warning for this object. I have modified the orientation limits to avoid the bright galaxy.
The flux density in a 3" aperture at the location of the BOA is 10^-16 erg/s/cm^2/AA. The corresponding flux density per arcsec^2 is 2.1e-17 erg/s/cm^2/AA/arcsec^2 (these are nominal fluxes assuming the background is zero). The brightest flux within a BOA aperture within the secondary search area is 6.9e-16 cgs.M77J2000J2000FUV=15.81 NUV=N/A F(1640)=1.6E-15erg/s/cm^2GALAXYSTARBURSTYESThe object gives a BOT warning for NUV acquisition but it is a clearly resolved galaxy. There are existing HST images of the field which confirms that this is an extended object.J2000J2000FUV=14.86 NUV=14.72 F(1640)=2.3E-15erg/s/cm^2GALAXYSTARBURSTYESThe BOT tool gives a health warning for the acquisition of this object but this is a resolved object, not a star.SBS1222+614J2000J2000FUV=16.17 NUV=15.91 F(1640)=6.1E-15erg/s/cm^2GALAXYSTARBURSTYESNGC3991NJ2000J2000FUV=14.65 NUV=14.55 F(1640)=3.7E-15erg/s/cm^2GALAXYSTARBURSTYESThe BOT gives an indication of health and safety problem on the source but the source is a clearly resolved galaxy thus this appears to be inaccurate.MRK0162J2000J2000FUV=15.82 NUV=15.72 F(1640)=3.3E-15erg/s/cm^2COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1589The scheduling data was generated by CASM 24.0.CASM was run in Phase II mode./private/var/folders/bj/l10yvm9m8xlgl2006s6gv0k00000gn/T/OPVisit805742486339285563.xml(Tic-Visit
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:dark-offset NIL
:dark-utilization 0
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:low-sky "N"
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)true30This has no space imaging but is likely also extended. However the exposure time is based on assuming a point source of u=16.4 (O3 star).The scheduling data was generated by CASM 24.0.CASM was run in Phase II mode./Users/jarle/Work/HST-COS/PhaseII/OP-cache/HeII-PhaseII-adjusted-angle-fixed-visit2-v10.xml(Tic-Visit
:proposal-id 14120
:visit-id "10"
:proposal-version -1
:trans-version "20160129"
:date "12-Apr-2016 23:34:49.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 261120
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 14120
:visit-id "10"
:obset-id "10"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 14120
:visit-id "10"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2946
:al-overhead-at-end 0
:internal-dur-at-end 67
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
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(Tic-Orbit
:proposal-id 14120
:visit-id "10"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3085
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:internal-dur-at-end 38
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
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)
(Tic-Orbit
:proposal-id 14120
:visit-id "10"
:orbit-number 3
:pcs-time 222
:si-vis-utilization 3085
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
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)true30No (useful) space imaging. Assuming a point source of u=17.1 gives the exposure time given