Resubmitting with new Orient Constraints for Visit 03 and adjusted ACQ times for S/N=40, now normalized to V-band mag.300798978----- Attempting Submission 1 (Thu Jul 29 13:55:29 GMT 2021) -----
----- Attempting Submission 2 (Thu Dec 02 19:43:32 GMT 2021) -----[CII], a High-z Diagnostic Diamond in the RoughIn order to fully characterize the high-z systems probed by JWST, it is essential that we prepare a robust rest-UV diagnostic toolkit to determine their physical and chemical properties. Crucially, such diagnostics must incorporate the element that emits strongest in the UV: carbon. Despite now having a suite of CIII], HeII, OIII], and CIV UV emission lines from high-z analogue systems at our fingertips from CLASSY, we are prevented from deriving accurate diagnostics because we lack a thorough understanding of the conditions affecting carbon emission in high-z environments. One key species is missing: [CII]. Here we propose to observe the [CII] 2325A multiplet in a sample of 12 CLASSY galaxies using STIS/G230L spectroscopy, thus building on pre-existing HST/COS spectroscopy to deliver essential insight into the diagnostic utility, production, and abundance of carbon. Our carefully chosen UV-emitting sample spans a wide range of high-z properties, including low-metallicity, high SFRs, and high ionization parameters. Using this important multiplet we will (i) provide the first empirical calibration of a highly-promising UV-based metallicity diagnostic, C23/HeII; (ii) decipher the ionization structure of C in each system by harnessing all of carbon's ionization stages (C+, C2+, C3+); (iii) derive highly accurate C/O abundances that do not rely on ionization correction factors (ICF); (iv) construct ICF grids for C to enable future C/O measurements in high-z systems. This study provides the first opportunity to thoroughly explore the origin of carbon in a range of high-z environments, thus exploiting its full potential as a chemical and physical diagnostic in the JWST era.We require STIS G230L MAMA observations in order to cover the 1570 - 3180 A wavelength range, fully encompassing the [C ii] 2325 multiplet (a blend of emission at 2323.50A, 2324.69A, 2325.40A, 2326.93A,and 2328.12A).
The prime science goals of this data involve the line ratios between several UV emission lines, several of which are in pre-existing COS data from the CLASSY program. As such, aperture matching between the STIS and COS data is imperative, especially for sources that are extended and/or show multi-component light profiles in the UV. To achieve this we match the position angle of the STIS slit to that of the COS observations (when achievable wrt the visibility of the object). If the objects are definitively point sources, no orient restriction is in place. We calculate ORIENT as PA+45deg, as stated in the STIS IHB. ORIENT restrictions for some targets have been significantly widened for some targets to enable schedulability.
In order to mitigate any issues with aperture losses we will match the width of the STIS slit (2" x 52") to the size of light profiles as measured from the COS NUV acquisition images,
thereby fully encompassing all of the NUV emission in each target.
2 point dither patterns along the slit are used to remove effects of hot pixels. We choose 0.3 arcsec spacing.
ETCs:
The STIS ETC was used to estimate exposure times necessary to reach a S/N~10 in the [C ii] 2325 multiplet using G230L. Previous emission line studies have shown
that this S/N is sucient to secure > 3 measurements. The [C ii] flux was estimated for each galaxy by using our (spatially matched) in-hand COS/FUV and optical SDSS data.
The predicted line strengths are given for each target to assist the CS in their ETC calculations, along with the continuum flux at 1900A observed in COS data.
For objects that are considered to be extended sources (i.e., light proles with > 0:6 GFWHM), we estimate the surface brightness of [C ii] using the C iii] and O iii] fluxes averaged over the 2.5" aperture area of COS. ETC simulations were performed using a flat continuum normalized to the 1900 A continuum flux observed by COS, superimposed with a [C ii] emission multiplet corresponding to the line flux (or surface brightness for extended sources) of each target at its observed wavelength.
We perform a standard target acquisition to obtain S/N=40 using CCD. Given that our science requirements can be achieved using the 52"2" STIS aperture, there is no need
to include an acquisition peak-up exposure. V-band magnitudes were used to normalize the SED for ACQ ETCs.
BOT Check:
GALEX clears for all exposures with coverage.
GSC2 reports violation for Visit 01 NUV MAMA - same field clears with Galex.
All targets have been previously observed with COS FUV+NUV and are deemed safe.To reduce, interpret, and delivery timely analysis of the STIS observations proposed here, we have compiled a team that is composed of world experts in UV observations (Aloisi, Berg, Bordoloi, Brinchmann, Erb, James, Hernandez, Kumari, Martin, Maseda, Nanayakkara). All members of our team have an excellent track record in leading, performing, analyzing, and publishing spectrscopic studies of star-forming galaxies, with several of our members leading multiple HST programs as PI (Aloisi, James, Erb, Berg, Kumari, Hernandez, Bordoloi, Martin).
The team consists of two current/previous STIS instrument scientists (Aloisi, Hernandez), with additional deep knowledge from the entire team on reduction techniques like wavelength calibration and fluxing of UV and optical spectroscopic data.
Scientifically, the team is uniquely qualified to pursue the range of science topics proposed here:
- Our team contain forefront leaders in UV emission line analysis (Berg, James, Mingozzi, Arellano-Cordova, Erb, Brinchmann, Nanayakkara, Martin, Maseda, Xu)
- We have etensive expertise in emission line modeling using photoionization codes such as CLOUDY and mappings (Berg, Erb, James, Arellano-Cordova, Nanayakkara, Amorin, Martin, Hernandez)
- Several are experts in chemical abundance analyses of star-forming galaxies (Aloisi, Berg, James, Hirschauer, Kumari, Arellano-Cordova, Mingozzi, Hernandez, Amorin, Maseda)
Our team is balanced with both pioneers of UV spectroscopy as well as new experts in the field. Moreover, the team is also anchored at both low-redshift and high-redshift such that we will design the proposed UV emission-line diagnostics with an eye towards what is observable by JWST.Galaxies6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYEMISSION LINE NEBULASTAR FORMING REGIONNONUV continuum is 5e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.1"
Predicted [CII] flux at 2325A = 3.22e-15 erg/s/cm^2MRK996J2000J2000GALAXYSTARBURSTNOThe coordinates for this target were obtained from a HLA image which is based on GSC2.3 astrometry.
NUV continuum is 4e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.5", multi-component light profile
Predicted [CII] flux at 2325A = 0.36e-15 erg/s/cm^2J2000J2000GALAXYEMISSION LINE NEBULASTAR FORMING REGIONNONUV continuum is 1e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3"
Predicted [CII] flux at 2325A = 0.05e-15 erg/s/cm^2J2000J2000GALAXYEMISSION LINE NEBULASTAR FORMING REGIONNONUV continuum is 1.25e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3", multi-component light profile
Predicted [CII] flux at 2325A = 0.26e-15 erg/s/cm^2J104457J2000J2000GALAXYEMISSION LINE NEBULASTAR FORMING REGIONNONUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.4", multi-component light profile in UV
Predicted [CII] flux at 2325A = 0.13e-15 erg/s/cm^2J2000J2000GALAXYEMISSION LINE NEBULASTAR FORMING REGIONYESNUV continuum is 5e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.7", extended source
Predicted [CII] flux at 2325A = 0.07e-15 erg/s/cm^2J2000J2000GALAXYEMISSION LINE NEBULASTAR FORMING REGIONNONUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.5"
Predicted [CII] flux at 2325A = 0.02e-15 erg/s/cm^2J2000J2000GALAXYEMISSION LINE NEBULASTAR FORMING REGIONNONUV continuum is 1e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.2"
Predicted [CII] flux at 2325A = 0.06e-15 erg/s/cm^2J132347J2000J2000GALAXYEMISSION LINE NEBULASTAR FORMING REGIONNONUV continuum is 3e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3", multi-component light profile
Predicted [CII] flux at 2325A = 0.11e-15 erg/s/cm^2LY52J2000J2000GALAXYEMISSION LINE NEBULASTAR FORMING REGIONNONUV continuum is 1e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3"
Predicted [CII] flux at 2325A = 0.2e-15 erg/s/cm^2J141851J2000J2000GALAXYEMISSION LINE NEBULASTAR FORMING REGIONNONUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.2"
Predicted [CII] flux at 2325A = 0.04e-15 erg/s/cm^2J2000J2000GALAXYEMISSION LINE NEBULASTAR FORMING REGIONYESNUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.4", multi-component light profile in UV
Predicted [CII] flux at 2325A = 0.1e-15 erg/s/cm^2J2000J2000STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/NUV-MAMASpectroscopicNoNoG230L2376POS-TARGDITHER0.3LINEfalsefalse290.0STIS-ALONG-SLIT2falseThe scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.Point source object, so no orientation constraints needed wrt COS observations (taken at PA=107 -> orient = 152,332)1657964326000249.04220775734086(Tic-Visit
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Predicted [CII] flux at 2325A = 3.22e-15 erg/s/cm^2NUV continuum is 5e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.1"
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Predicted [CII] flux at 2325A = 0.36e-15 erg/s/cm^2NUV continuum is 4e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.5", multi-component light profile
Predicted [CII] flux at 2325A = 0.36e-15 erg/s/cm^2The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.Point source object, so no orientation constraints needed wrt COS observations (taken at PA=326 -> orient = 11,191)164586577500025.0(Tic-Visit
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Predicted [CII] flux at 2325A = 0.05e-15 erg/s/cm^2NUV continuum is 1e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3"
Predicted [CII] flux at 2325A = 0.05e-15 erg/s/cm^2The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.Adding a series of orient restraints to align with archival COS data1653388821000130.0(Tic-Visit
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Predicted [CII] flux at 2325A = 0.26e-15 erg/s/cm^2NUV continuum is 1.25e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3", multi-component light profile
Predicted [CII] flux at 2325A = 0.26e-15 erg/s/cm^2The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.1645122899000226.0(Tic-Visit
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Predicted [CII] flux at 2325A = 0.13e-15 erg/s/cm^2NUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.4", multi-component light profile in UV
Predicted [CII] flux at 2325A = 0.13e-15 erg/s/cm^2The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.1647066956000260.0(Tic-Visit
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Predicted [CII] flux at 2325A = 0.07e-15 erg/s/cm^2NUV continuum is 5e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.7", extended source
Predicted [CII] flux at 2325A = 0.07e-15 erg/s/cm^2The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.1652223289000166.0(Tic-Visit
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)true10NUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.5"
Predicted [CII] flux at 2325A = 0.02e-15 erg/s/cm^2NUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.5"
Predicted [CII] flux at 2325A = 0.02e-15 erg/s/cm^2The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.No orient constraints required to align with COS observations since object is considered point source1651354605000158.9186940956215(Tic-Visit
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Predicted [CII] flux at 2325A = 0.06e-15 erg/s/cm^2NUV continuum is 1e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.2"
Predicted [CII] flux at 2325A = 0.06e-15 erg/s/cm^2The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.(Tic-Visit
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)false10NUV continuum is 3e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3", multi-component light profile
Predicted [CII] flux at 2325A = 0.11e-15 erg/s/cm^2NUV continuum is 3e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3", multi-component light profile
Predicted [CII] flux at 2325A = 0.11e-15 erg/s/cm^2The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.No orient constraints required to align with COS observations since object is considered point source1655584468000128.2535395417351(Tic-Visit
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)true10NUV continuum is 1e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3"
Predicted [CII] flux at 2325A = 0.2e-15 erg/s/cm^2NUV continuum is 1e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3"
Predicted [CII] flux at 2325A = 0.2e-15 erg/s/cm^2The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.No orient constraints required to align with COS observations since object is considered point source(Tic-Visit
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:data-volume 296080
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16692
:visit-id "Z1"
:obset-id "Z1"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16692
:visit-id "Z1"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2763
:al-overhead-at-end 0
:internal-dur-at-end 440
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3157
:pcs-gap 0
)true10NUV continuum is 1e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3"
Predicted [CII] flux at 2325A = 0.2e-15 erg/s/cm^2NUV continuum is 1e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.3"
Predicted [CII] flux at 2325A = 0.2e-15 erg/s/cm^2The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.No orient constraints required to align with COS observations since object is considered point source1655338712000137.10000000000002(Tic-Visit
:proposal-id 16692
:visit-id "11"
:proposal-version -1
:trans-version "20210514"
:date "02-Dec-2021 14:27:14.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 296080
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16692
:visit-id "11"
:obset-id "11"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16692
:visit-id "11"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2749
:al-overhead-at-end 0
:internal-dur-at-end 440
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3142
:pcs-gap 0
)true10NUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.2"
Predicted [CII] flux at 2325A = 0.04e-15 erg/s/cm^2NUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.2"
Predicted [CII] flux at 2325A = 0.04e-15 erg/s/cm^2The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.1655333282000160.0(Tic-Visit
:proposal-id 16692
:visit-id "12"
:proposal-version -1
:trans-version "20210514"
:date "02-Dec-2021 14:27:15.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 296080
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16692
:visit-id "12"
:obset-id "12"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16692
:visit-id "12"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2751
:al-overhead-at-end 0
:internal-dur-at-end 440
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)true10NUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.4", multi-component light profile in UV
Predicted [CII] flux at 2325A = 0.1e-15 erg/s/cm^2NUV continuum is 2e-15 erg/s/cm^2/A at 1900A from COS observations, FWHM=0.4", multi-component light profile in UV
Predicted [CII] flux at 2325A = 0.1e-15 erg/s/cm^2