0Assigned ID: 2630
----- Attempting Submission 1 (Tue Oct 12 18:19:35 GMT 2021) -----
HST Phase I Proposal 2630 successfully submitted.
Receipt: # 2630-10----- Attempting Submission 1 (Mon Oct 11 22:00:17 GMT 2021) -----
HST Phase II Proposal 16843 successfully submitted.
Receipt: # 16843-1
----- Attempting Submission 2 (Wed Oct 13 21:54:59 GMT 2021) -----
----- Attempting Submission 4 (Mon Oct 18 17:49:13 GMT 2021) -----UVIS FLASH is based on ETC calculations and chosen to have at least 20 e- per pixel to avoid poor CTE.Dwarf Galaxies with Radio-Selected (and Sometimes Wandering) Massive Black HolesUsing high-resolution observations from the Very Large Array, Reines et al. (2020) discovered a set of compact radio sources in nearby dwarf galaxies with luminosities indicative of accreting massive BHs. Moreover, many of these radio sources are not in the centers of the galaxies with offsets as large as ~4'' (~2 kpc). We propose Chandra and HST observations of 8 dwarf galaxies hosting radio-selected massive BHs to 1) firmly establish the presence of massive BHs (some of which are `wandering') in these dwarf galaxies and characterize the compact X-ray emission from the BHs, 2) place some constraints on the BH masses and Eddington ratios, and 3) search for stellar counterparts of the BHs and determine spatially-resolved star formation rates in the host galaxies.We will obtain HST/WFC3 observations in three filters, including UVIS narrow-band H-alpha imaging (F680N or F665N depending on redshift) and wide-band continuum imaging in F475W and F814W. We choose the wideband filters to bracket the wavelength of H-alpha (for continuum subtraction) and to obtain color information. We can achieve our science goals with one HST orbit per galaxy for a total of 8 orbits.
From prior experience, exposure times are based on detecting a 5 Myr-old, ~10^5 Msun star cluster in our most distant target galaxy (z =0.05) with a signal-to-noise ratio of S/N=10. Starburst99 models of an instantaneous burst indicate that the corresponding H-alpha flux is ~10^-16 erg/s/cm^2 with an underlying continuum flux density of ~5 x 10^-19 erg/s/cm^2/Ang. Assuming the cluster is a point source, the WFC3/UVIS exposure time calculator suggests we need ~17 minutes in F680N. The required times in F475W and F814W are ~8 and ~ 9 minutes, respectively. Note that we have also allowed for 1 magnitude of visual extinction (AV = 1 mag) in these calculations. We will break the total time into two dithered exposures to improve the PSF sampling and avoid bad pixels, as well as include a post flash to avoid poor charge efficiency. We will use the UVIS 1k x 1k subarray (to avoid buffer dumps) with the more efficient chip 2. Our galaxies are quite compact so using a subarray will not compromise our science or limit our sky subtraction.PI Reines is an Assistant Professor at Montana State University. Reines is an expert on massive BHs in dwarf galaxies, AGNs, and extreme star formation. She uses imaging and spectroscopy in her analysis, and is regular user of Chandra, HST and the VLA. She is the PI of 4 accepted Chandra proposals and has published more than 20 papers using data from NASA telescopes. Reines will be responsible for the scientific and administrative conduct of the proposed project. A graduate student working under the advisement of Reines will lead the analysis and publication of the proposed observations.
Co-I Molina is postdoctoral researcher working with PI Reines at Montana State University. Molina is an expert in extragalactic star formation and AGNs (especially LINERS) and recently published a follow-up paper on the Reines et al. (2020) sample entitled "Outflows, Shocks and Coronal Line Emission in a Radio-Selected AGN in a Dwarf Galaxy".
Co-I Bogdan is an astrophysicist at the Smithsonian Astrophysical Observatory. His expertise is in high energy astrophysics, supermassive black holes, and hot gas in galaxies, groups and clusters.
Co-I Kraft is an astrophysicist at the Smithsonian Astrophysical Observatory and Project Scientist for the Chandra High Resolution Camera (HRC). He is also the Principal Investigator (PI) for the science instrument.
Co-I Darling is a Professor at the University of Colorado. He studies black holes, galaxies and cosmology, and is an expert radio astronomer.
Co-I Condon is a radio astronomer at NRAO with expertise in AGNs and galaxies.Supermassive Black Holes and Active Galaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTMAGELLANIC IRREGULARYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYDWARF COMPACTMAGELLANIC IRREGULARYESJ2000J2000GALAXYDWARF COMPACTMAGELLANIC IRREGULARYESJ2000J2000GALAXYDWARF COMPACTMAGELLANIC IRREGULARYESJ2000J2000GALAXYDWARF COMPACTMAGELLANIC IRREGULARYESJ2000J2000GALAXYDWARF COMPACTMAGELLANIC IRREGULARYESJ2000J2000GALAXYDWARF COMPACTMAGELLANIC IRREGULARYESJ2000J2000GALAXYDWARF COMPACTMAGELLANIC IRREGULARYESJ2000J2000WFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF680NWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF665NWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF680NWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF680NWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF680NWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF680NWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF680NWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF680NWFC3/UVISImagingNoNoF814WPOS-TARGDITHER0.145LINEfalsefalse246.84WFC3-UVIS-DITHER-LINE1falseThe scheduling data was generated by CASM 29.2.CASM was run in Phase II mode./Users/amyreines/Proposals/Chandra/cycle23_radiodwarfs/HST/APT_jointHST_F814W/OP-cache/jointHST_final-v01.xml(Tic-Visit
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