0Assigned ID: 2412
----- Attempting Submission 1 (Fri Apr 09 23:01:14 GMT 2021) -----FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser0----- Attempting Submission 1 (Wed Jul 21 21:45:17 GMT 2021) -----
HST Phase II Proposal 16661 successfully submitted.
Receipt: # 16661-1
----- Attempting Submission 2 (Mon Aug 16 23:03:17 GMT 2021) -----I did run the Target Confirmation Tool and it looks good. But APT kept crashing.
I adjusted the post-flash based on ETC runs. APT still gives warnings though.Dwarf Galaxies with Radio-Selected Massive Black HolesStudies of massive black holes (BHs) in nearby dwarf galaxies can provide important constraints on the birth and growth of the first seed BHs in the early Universe. Using 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, some of these radio sources are not in the centers of the galaxies with offsets on the order of ~1 kpc. As part of a pilot study, we propose HST/WFC3 observations of 3 dwarf galaxies hosting radio-selected (''wandering'') massive BHs that also have guaranteed X-ray observations with Chandra. We propose narrow-band H-alpha imaging and wide-band optical continuum imaging to 1) determine spatially-resolved star formation rates and colors, 2) search for faint, small optical counterparts of the BHs, and 3) determine detailed morphologies of the dwarf host galaxies. The proposed observations are crucial to asses possible contributions from star-formation-related emission at X-ray and radio wavelengths, and characterize the properties of this new class of BH-hosting dwarf galaxies.We will obtain HST/WFC3 UVIS observations in three filters, including narrow-band H-alpha imaging (F680N) and wide-band continuum imaging at 4300 Ang (F438W) and 8000 Ang (F814W). We choose the F438W and F814W filters to bracket the wavelength of H-alpha (for continuum subtraction) and to avoid strong emission lines such as [OIII] 5007 and the [OII] 3727, 3729 doublet. We have three target galaxies and can achieve our science goals with two HST orbits per galaxy for a total of 6 orbits.
From prior experience, exposure times are based on detecting a 5 Myr-old, ~3x10^4 Msun star cluster at the distance of our target galaxies (z ~ 0.02-0.03) 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 ~3 x 10^-19 erg/s/cm^2/Ang. Assuming the cluster is a point source, the WFC3/UVIS exposure time calculator suggests we need ~35 minutes in F680N. The required times in F814W and F438W are ~13 and ~ 11 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 four 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 2k x 2k 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. A similar observing strategy has been successfully employed in previous work (Kimbro et al. 2021).
To summarize, we can achieve our science goals with 2 orbits per galaxy. We will spend one orbit on narrow-band H-alpha imaging (F680N) and one orbit on wide-band continuum imaging (F438W and F814W). Our observing strategy provides the requisite time on source in each filter, as well as sufficient time for acquisition and instrument overheads (including guide-star acquisition, readout and dithering).PI Reines is an Assistant Professor at Montana State University. Reines is an expert on supermassive black holes in dwarf galaxies, AGNs, and extreme star formation. She uses imaging and spectroscopy in her analysis, and is regular user of HST, Chandra, and the VLA. She has analyzed observations from many HST instruments, including NICMOS, WFPC2, ACS, WFC3, and STIS. She is the PI of 5 accepted HST proposals, and has published ~20 papers using data from NASA telescopes.
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). She has experience analyzing spatially-resolved spectra, including calibrating the spectra, modeling and decomposing the continuum, measuring the emission lines, and comparing the measurements to photoionization and shock models (Molina et al. 2018). In particular, she has expertise in working with large data sets from both long-slit and integral field spectroscopy (e.g., with HST/STIS and SDSS-IV/MaNGA), and well as multi-wavelength photometry.
Co-I Darling is a Professor at the University of Colorado. He studies black holes, galaxies and cosmology, and is an expert radio astronomer.Supermassive Black Holes and Active GalaxiesGalaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTINTERACTING GALAXYRADIO GALAXYJ2000J2000GALAXYDWARF COMPACTINTERACTING GALAXYRADIO GALAXYJ2000J2000GALAXYDWARF COMPACTINTERACTING GALAXYRADIO GALAXYJ2000J2000WFC3/UVISImagingNoNoF680NWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF680NWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF680NWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF438WPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT3false/private/var/folders/z3/xy_g1v_s5fz9yrhzb8thz4cr0001qc/T/OPVisit1475008518790201261.xmlThe scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.(Tic-Visit
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