Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.0Assigned ID: 3046
----- Attempting Submission 1 (Thu Mar 24 19:34:55 GMT 2022) -----
HST Phase I Proposal 3046 successfully submitted.
Receipt: # 3046-1These have all been checkedORBITAL VISIBILITY OVERRUN
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ORBITAL VISIBILITY OVERRUN
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.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
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INEFFICIENT ORDERING OF FP-POS POSITIONS
ORBITAL VISIBILITY OVERRUN
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ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
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.
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.
INEFFICIENT ORDERING OF FP-POS POSITIONS
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
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INEFFICIENT ORDERING OF FP-POS POSITIONS
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUNRe-submitted with repeats of:
Visit 4 -> split into 54 and 64. Due to extended target, orientation of 54 has been tied to 64.
Visit 8 -> now 58.
New submission accounts for RGM.-1042222684----- Attempting Submission 1 (Thu Jul 14 19:42:21 GMT 2022) -----
----- Attempting Submission 2 (Tue Aug 30 18:15:11 GMT 2022) -----
----- Attempting Submission 3 (Thu Sep 15 16:36:59 GMT 2022) -----
----- Attempting Submission 4 (Thu Sep 15 22:11:42 GMT 2022) -----
----- Attempting Submission 5 (Fri Jun 14 15:25:58 GMT 2024) -----Use of less than 4 FP-POS is warranted given the low S/N
The risks involved with the >2400s G160M observations are minimalSharpening our High-z Toolset: Spatially Resolving UV Emission Line Diagnostics Throughout Pristine GasIt is imperative that we enter the high-z era with a diagnostic toolset that enables us to decipher the chemical and physical conditions of a galaxy using primarily UV emission lines. Moreover, this toolset needs to be most effective in typical high-z environments (low metallicity, hard ionising fields). Unfortunately, current efforts to derive such a toolset suffer from severe paucity in the extremely metal-poor (XMP) regime (<5% Zsol), and - most importantly - globally integrated spectra that are prone to large observational biases. Local high-z analogs are rare, particularly in the XMP regime, and very few allow us to examine how integrated spectra can bias the derived diagnostics. Here we have a unique opportunity to solve these issues by observing 5 individual HII regions throughout a chemically inhomogeneous, XMP star-forming galaxy, DDO68, with HST/COS, covering all of the key UV diagnostic lines (CIV, HeII, OIII], & CIII]). Each region has MOS optical spectroscopy, providing the first spatially resolved UV-to-optical coverage across a range of metallicities and ionizing field strengths. The HII regions provide independent samples within DDO68 to accurately calibrate UV lines using photoionization models for individual ionized nebulae, unlike integrated light studies. This exquisite dataset will allow us to first understand the physical properties driving UV lines, then harness this knowledge to provide stand-alone UV diagnostics for metallicity, density, and ionization source. Our parameter space ensures that we can accurately calibrate the UV diagnostics in a range of primordial-like environments, thereby providing the best UV toolset possible for the high-z era.The program observes 6 separate HII regions in the extremely metal poor galaxy, DDO68.
The combination of the COS G160M+G185M gratings covers all the UV emission lines necessary for robust metallicity and excitation determination (C iv, O iii], He ii, C iii]).
For the NUV, we utilize G185M/1913 to optimize the throughput coverage at the position of the emission line C iii] within stripe B.
In the FUV, G160M/1533 was chosen to optimize the throughput for the C iv, He ii and O iii] emission (on Segment B), with only a 100 A featureless gap until G185M/1913.
Following the COS IHB, our number of exposures per orbit are such that G160M will be executed at its new default lifetime position (LP6).
We will utilize 4 FP-POS positions for G185M and 3 FP-POS for G160M to maximize S/N. The use of 3 FP-POS for G160M is within the S/N guideline requirements set out in the IHB
ETCs: Exposure time calculations (ETCs) were based on obtaining S/N~3-5 (per spectral resolution element) in O iii] 1666A for G160M and C iii] 1909A for G185M.
Fluxes in O iii] 1666A and C iii] 1909A were predicted from Te values and [O iii] 5007A flux for each Hii region (accounting for E(B-V) values), and the observed C/O ratio of dwarf galaxies. Continuum fluxes of 8E-16 and 7E-16 erg/s/cm2/A at 1600 and 1900|A, respectively, measured using the archival G160M+G185M observations of DDO68-1 (PID: 13788), were used for G160M and G185M ETCs, respectively.
All fuxes used for the ETCs can be found in Table 2 of the Phase I document or the visit level comments
Owing to the faintness of our emission lines, the continuum levels are the main drivers of our exposure times.
ACQ/IMAGE target acquisition times were calculated for a (recommended) S/N~20. All targets will be offset from a compact HII region to ensure the COS aperture remains positioned on the ionized gas in each cluster rather than the cluster itself. After the ACQ/IMAGE on the 'offset region', we take an NUV image of the target cluster to inspect the cross-dispersion profile of the cluster (required for any absorption line fitting) before taking the spectroscopic observations.
The 'offset region' has a flux measured within r=0.4" aperture on F275W WFC3 image of 4.873E-20 erg/s/cm^2/A, ABmag=20.2
The coordinates for each HII region were taken from the HAP processed images, which use GAIA astrometry. We used ACS F658N (for the G160M and G185M exposures) to align with the ionized gas. For the TACQ of the offset star, we utilized WFC3 UVIS F275W.
The ETC reported no warnings for violations of the local and/or global bright object limits.Several members of our team are experts in the field of UV spectroscopy (Dr Bethan James, Dr Danielle Berg,
Dr Alessandra Aloisi, Dr Swara Ravindranath, Dr Svea Hernandez, Dr Nimisha Kumari, Dr Valentina Abril Melgarejo, Dr. Mingozzi, Dr Alec Hirschauer), each having significant experience with HST/COS spectroscopy in particular. They have lead several HST/COS observing campaigns, with 9 papers published in the past 5 years on data carried out with COS observations.
Dr Bethan James is currently the deputy lead of the HST/COS team, Dr Alessandra Aloisi was the COS+STIS team lead 2006-2013, Dr Alec Hirschauer, Dr Nimisha Kumari and Dr Svea Hernandez are current/previous members of the HST/COS team. As such they are all intimately familiar with all aspects of the COS instrument, its data analysis and observations.
Dr Bethan James, Dr Danielle Berg, Dr Alec Hirschauer & Dr Matilde Mingozzi are experts in determining chemical abundances and physical conditions from UV-to-optical emission lines, primarily focussing on low-metallicity star-forming galaxies.
Dr Bethan James, Dr Nimisha Kumari, Dr Matilde Mingozzi and Dr Valentina Abril Melgarejo specialize in spatially-resolved spectroscopy over the UV-to-optical wavelength range.
Dr Danielle Berg & Dr Swara Ravindranath are experts in photoionization modeling, and have pioneered much of the work concerning UV emission line diagnostics. Such models will be crucial in interpreting the data from this proposal.
Dr Francesca Annibali, Dr Elena Sacchi, and Dr Alessandra Aloisi, are all experts in the field of star-formation and stellar populations in nearby dwarf galaxies. Between them, they have lead several observing campaigns (one of which with HST ACS/WFC3 imaging) to observe DDO68 (the target of this proposal). They have published 4 papers concerning DDO68 during the past 3 years and are intimately familiar with DDO68. Dr Francesca Annibali is the PI for the (in-hand) LBT MOS optical spectroscopic observations which are critical for the science goals described here.Galaxies6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTAR FORMING REGIONYESF275W WFC3 ABmag = 19.575J2000F@3600A 6e-17 erg/s/cm^2/AGALAXYDWARF COMPACTSTAR FORMING REGIONNOF275W WFC3 ABmag = 20.375J2000F@3600A 1e-16 erg/s/cm^2/AGALAXYDWARF COMPACTSTAR FORMING REGIONYESF275W WFC3 ABmag = 21.014J2000F@3600A 2.5e-17 erg/s/cm^2/AGALAXYDWARF COMPACTSTAR FORMING REGIONNOF275W WFC3 ABmag = 20.46J2000F@3600A 2e-17 erg/s/cm^2/AGALAXYDWARF COMPACTSTAR FORMING REGIONNOF275W WFC3 ABmag = 21.29J2000F@3600A 1e-17 erg/s/cm^2/AISMHII REGIONNOFlux measured within r=0.4" aperture on F275W WFC3 image: 4.873E-20 erg/s/cm^2/A
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2.89E-17 (1666A)
1.50E-15 (1909A)
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continuum fux of 8x10^-16 and 7x10^-16 erg/s/cm2/A at 1600A and 1900A(Tic-Visit
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2.48E-17 (1666A)
1.31E-16 (1909A)
continuum fux of 8x10^-16 and 7x10^-16 erg/s/cm2/A at 1600A and 1900A1677241427000132.31(Tic-Visit
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2.48E-17 (1666A)
1.31E-16 (1909A)
continuum fux of 8x10^-16 and 7x10^-16 erg/s/cm2/A at 1600A and 1900A1709982713000132.31(Tic-Visit
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)true33The scheduling data was generated by CASM 32.1.CASM was run in Phase II mode./Users/bjames/Documents/observing_proposals/COS_0322/COS_Emission/OP-cache/17125_phaseII_hopr_visits_4_8-v58.xmlPredicted fluxes used for ETC: erg/s/cm^2/A
2.48E-17 (1666A)
1.31E-16 (1909A)
continuum fux of 8x10^-16 and 7x10^-16 erg/s/cm2/A at 1600A and 1900A(Tic-Visit
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