0Assigned ID: 750
----- Attempting Submission 1 (Fri Mar 06 20:37:09 GMT 2020) -----COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
LIFETIME-POS is required with G130M when not in Supported mode.
LIFETIME-POS is required with G130M when not in Supported mode.
LIFETIME-POS is required with G130M when not in Supported mode.
LIFETIME-POS is required with G130M when not in Supported mode.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
LIFETIME-POS is required with G130M when not in Supported mode.
ORBITAL VISIBILITY OVERRUN
INEFFICIENT ORDERING OF FP-POS POSITIONS
REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE
REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE
REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE
REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE
REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE
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.Resubmitting after splitting 6 orbit visit into two 3 orbit visits.
Also added details on BOP checking.
============
Resubmitting after selecting LP4 for Visit 06
This required 'restricted mode' since this option wasn't selectable in available mode
LIFETIME_POS was required because LP5 will be used for 1291 observations after Oct 4 2021 and I require LP4.-1246925668----- Attempting Submission 2 (Wed Sep 23 20:07:26 GMT 2020) -----
----- Attempting Submission 3 (Wed Sep 29 20:16:16 GMT 2021) -----Please see previous submission for explanation of warnings/errors.Pinning down multi-phase mixing of metals within star-forming galaxiesTreating metals as homogeneous distributions throughout star-forming galaxies (SFGs) is no longer acceptable. Chemical inhomogeneities have been detected in the ionized gas of numerous SFGs via spatially resolved studies, with large implications for the flow of metals within and around galaxies. However, metals exist in multiple phases and, at present, the spatial distribution of metals throughout the neutral gas in SFGs remains unknown. Recent high-resolution galaxy-scale hydrodynamical simulations have made significant advancements, opening up crucial questions concerning mixing timescales and the presence of localized enrichment between the two gas phases. Answers can only be found by measuring both the neutral and ionized gas abundances along multiple identical sightlines throughout a nearby SFG. Here we propose COS G130M spectroscopy of 6 sightlines in NGC5253 (4 new, 2 archival), to measure the neutral gas abundances towards clusters ranging between 1-15Myr. When combined with ionized gas abundances of spatially matched spectra from VLT/MUSE, this unique dataset will provide the first spatially resolved study of metals both within and between two phases within a galaxy. Determining whether metal abundance offsets exist between the two phases, both globally and locally across a range of HII region properties, enables an exceptionally detailed sampling of chemical mixing scenarios and enrichment mechanisms experienced in SFGs. NGC5253's low-metallicity and high SFR make our findings applicable to both nearby and high-z SFGs. This remarkable study will provide the first observational test of multi-phase abundance patterns in cosmological simulations of dwarf galaxies.Science overview: We propose to perform COS/FUV G130M/1291 and G130M/1222 spectroscopy of 4 pointings throughout a nearby, low-metallicity, star forming galaxy, NGC 5253. By combining this data with 2 pointings towards NGC 5253 from archival data (PIDs 11579, 15193), this dataset will allow us to map the neutral gas abundances towards 6 HII regions throughout NGC 5253. Furthermore, via in-hand optical integral field spectroscopic observations of NGC 5253 from VLT-MUSE, this unique dataset will offer the first spatially matched UV+optical spectroscopic study of a nearby SFG - enabling us to accurately compare the neutral and ionized gas abundances along the same sightline for a variety of stellar properties.
Settings: We require G130M/1291 observations in order to cover the 1132-1433A spectral range. This provides access to a wide selection of ISM lines, required to determine the column densities of CII, NI, OI, SII, SiII, FeII, PII, while also covering the Lya region - essential in computing the neutral hydrogen column density (N(HI)) required for neutral gas abundances. We additionally request coverage of the 1070-1363A range using G130M/1222. This allows us to cover the FeIII 1122 line, required to calculate the ionization state of the gas via the FeIII/FeII line ratio.
Sources:
All targets are considered to be extended sources, with the exception of Cluster 8
For the pointings with multiple resolved clusters in the aperture (C9+10, C5+11) we have chosen an orient such that the clusters are separated in the cross-dispersion direction. Details are given in visit description boxes.
For the pointing covering clusters 1+2+3+4, we will orient along 1+2+4, excluding cluster 3, to allow for the minimal amount of blending.
For pointing coordinates, please use the HLSP data of NGC5253 (aligned to Gaia astrometry), which can be found at http://archive.stsci.edu/hlsp/ngc5253-dr2
ETCs: The COS spectroscopic ETC was used to estimate exposure times necessary to reach a S/N 7 at 1150A for G130M/1222 and G130M/1291. The flux of each target was normalized to the total observed flux that resides within the COS aperture, as measured on the HST/ACS/SBC/F125LP image (Table 1). For those pointings where several clusters are covered by the COS aperture, the flux corresponds to the average flux density across the aperture.
BOP: The ETC reported no warnings for violations of the local and/or global bright object limits, so we expect the targets to be safe to observe. APT/BOT/GALEX gives local rate violation for one point (in PSA), global B exceeded with 1.86e4 counts/s. All counts rates are for GALEX GII magnitudes. All stars within the field are safe, as shown via ETCs for SCI, ACQ, and NUV imaging. A document with supporting information can be supplied to the CS. The same violation point was safely observed by Visit 06 of 15193 and in 11579.
The spectroscopic exposures in each pointing will be executed with FP-split.
TACQ: We will use the standard target acquisition (TA) strategy and perform ACQ/IMAGE TA with an ETC estimate to provide the (recommended) S/N 20. For pointings with multiple resolved clusters within the aperture, we will use affixed offset target acquisition from a nearby FUV-bright source, followed by a NUV image.Several members of our team are experts in the field of UV spectroscopy (Dr Bethan James, Dr Alessandra Aloisi, Dr Svea Hernandez, Dr Nimisha Kumari).
Dr Bethan James, Dr Alessandra Aloisi, Dr Svea Hernandez, and Dr Nimisha Kumari have significant experience with HST/COS spectroscopy in particular. They have lead several HST/COS observing campaigns, with 5 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 team lead 2006-2013, Dr Nimisha Kumari is currently a member of the COS team, and Dr Svea Hernandez was a member of the HST/COS team 2012-2014. As such they are all intimately familiar with all aspects of the COS instrument, its data analysis and observations.
Dr Bethan James, Dr Alessandra Aloisi and Dr Svea Hernandez are experts in determining chemical abundances from FUV spectra and photoionization modelling of HII regions.
Dr Bethan James and Dr Nimisha Kumari are experts in optical emission line spectroscopy, primarily focussing on low-metallicity star-forming galaxies. They both specialize in spatially-resolved spectroscopy over the UV-to-optical wavelength range and are highly experienced with VLT/MUSE observations.
Dr Alessandra Aloisi is an expert in the field of star-formation and stellar populations in nearby dwarf galaxies.
Dr Andrew Emerick is an expert in galaxy-scale hydrodynamical simulations of star-forming dwarf galaxies. He has pioneered this field, designing models where multi-phase chemical mixing is sampled at ultra-high spatial resolution, publishing several studies over the last few years. His work has focused primarily on the distribution of metals in simulated dwarf galaxies.Galaxies6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTELLAR CLUSTERSTAR FORMING REGIONYESFlux = average flux within COS 2.5" apertureJ2000F(125LP)=2E-15 erg/s/cm^2/ASTELLAR CLUSTERSTAR FORMING REGIONYESFlux = average flux within COS 2.5" apertureJ2000F(125LP)=1.79E-16 erg/s/cm^2/ASTELLAR CLUSTERSTAR FORMING REGIONNOHLA ACS/SBC F125LP image used for coordinates
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