For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.0Assigned ID: 6830
----- Attempting Submission 1 (Thu Apr 10 23:22:19 GMT 2025) -----
HST Phase I Proposal 6830 successfully submitted.
Receipt: # 6830-1We have reviewed the COS documentation and will use G160M in the LP6 setupmodified FP-POS in COS orbits. G130M/1291 now has 3 and 4, G160M/1589 set to all with 4 subexposures in only 1 main exposure (reduced from 2)-242003209----- Attempting Submission 1 (Fri Aug 08 22:29:36 GMT 2025) -----
HST Phase II Proposal 18111 successfully submitted.
Receipt: # 18111-1
----- Attempting Submission 2 (Mon Aug 25 18:40:16 GMT 2025) -----
----- Attempting Submission 3 (Tue Aug 26 14:26:39 GMT 2025) -----
----- Attempting Submission 4 (Thu Jun 11 18:20:49 GMT 2026) -----Ultraviolet Spectroscopy and Optical Imaging of 4 Local Broad-Line Blue Compact Galaxies, Which Resemble Distant Little Red DotsBlue Compact Dwarf (BCD) galaxies are a unique class of low-mass, low-metallicity, gas-rich, high star formation rate systems. A small subset have been found in the local Universe (z=0.1-0.3) to exhibit persistent broad emission lines (BL-BCDs) and concave SEDs indicative of hosting obscured AGN, potentially with overmassive supermassive black holes. These BL-BCDs lack strong hard X-ray emission, show little optical variability, and have extreme blueshifted H and He absorption features, challenging traditional AGN diagnostics. Intriguingly, many high-redshift `little red dots' (LRDs) found by JWST show similar characteristics. We propose to acquire far-UV spectra and 3-color WFC3/UVIS imaging for a sample of four well characterized BL-BCDs. These data will better elucidate the contributions from the AGN and stellar population and potentially provide critical input on a number of uncertain properties of BL-BCDs, and by extension, distant LRDs.We propose to observe the sample of four BL-BCD with both HST COS GL130M + GL160M and WFC3 UVIS F300X, F475W, and F850LP. While high S/N optical and NIR spectral constraints on BL-BCDs can be performed from the ground, these have thus far offered ambiguous constraints, possibly due to the stronger influence from the AGN. The proposed UV spectral and spatially resolved studies of faint compact emission are well-suited to HST's capabilities in space. Based on the high Balmer decrements, low metallicities and existing rest-frame UV spectra of BL-LRDs with JWST, we may expect that the UV regime of BL-BCDs may lack most broad and/or bright lines, aside from Ly-alpha and perhaps HeI and HeII. Instead, if the UV is dominated stellar light from a nuclear star cluster, we expect to see FUV signatures of very young stellar populations, namely, stellar absorptions.
For COS, we will use the two medium-resolution gratings, G130M and G160M (lam_cen=1291 and 1589, respectively) to cover the almost continuous spectral coverage between Ly-alpha and HeII (1640A), i.e., 1130--1780\AA with a few (short) gaps. We adopt a combination of G130M+G160M rather than a single setup with G140L because (i) each of them provides almost a 2x better throughput, so after binning along the wavelength we will get similar quality of continuum measurements; (ii) they provide much higher spectral resolution, which is crucial for the detection of narrow blue-shifted absorption lines associated with outflows, as we expect for our targets.
For UVIS WFC3, we will use F300X+F475W+F850LP to probe the faint extended emission associated with the underlying older stellar population, enabling constraints on the stellar mass, age, and morphology of the hosts. These particular filters were chosen so as to mitigate contamination from high-EW lines in the nucleus, the PSF of which we will need to model and remove. The latter motivates us to adopt 3 UVIS bands, which offer a somewhat better sampled PSF compared to the IR detector. Notably, F300X will probe young stars in the NUV, and is 3 times more efficient than F275W for the same exposure time. F850LP will probe a redder starlight to offer a useful upper limit on stellar mass, while avoiding H-alpha and HeI 10830A. F850LP will also serve as the primary filter for the two-dimensional light profile decomposition to estimate structural properties (dust attenuation is not considered important here vs. the bluer bands, while the width of the instrumental PSF is still small). F475W (SDSS g) will be crucial for the analysis of stellar population properties of host galaxies in a combination with F850LP, while avoiding H-beta+[O III] and only suffering minor continuum contamination from weaker Balmer lines and [O II].PI FB has extensive experience in multiwavelength studies of AGN and hosts, including optical spectral and photometric observations, and has led or co-authored several hundred works on AGN to date, with several being closely related to the aim of the current proposal.
Co-I IC is a research scientist at Harvard-Smithsonian Center for Astrophysics (USA). He is a specialist in dwarf galaxies, compact galaxies, stellar populations, and AGN with the emphasis on active intermediate-mass black holes.
co-I KG is a graduate student at Universite de Paris (France); IC, and KG published the sample of intermediate-mass black holes (Chilingarian et al. 2018 ApJ 863 1), which ended up in the top-3% most cited papers published in 2018; and first spatially resolved stellar population profiles for ultra-diffuse dwarf galaxies (Chilingarian et al. 2019 ApJ 884 79) pushing the limits of low-surface brightness galaxy studies using integrated light spectra, which ended up in the top-5% most cited papers published in 2019. Later, they published a paper in Nature Astronomy (Grishin et al. 2021) about the formation of ultra-diffuse galaxies in clusters via ram pressure stripping.
co-I BR is a graduate student supervised by FB.
Co-Is ER is a student supervised by IC.
Our team has a 20-yr long expertise in reducing, analyzing, and publishing data from all major optical/IR ground-based observatories (Keck, ESO VLT, Gemini, MMT, Las Campanas) and also sub-mm facilities (ALMA, NOEMA). This project is a part of our large multi-wavelength campaign on studies of small black holes in dwarf galaxies and/or intermediate-mass black holes, which includes new X-ray observations with Chandra, ground-based spectroscopy with Keck, VLT, and Magellan telescopes, archival research using VLA data in the radio, and analysis of optical light curves. We are also currently running a snapshot survey with the HST, which targets a large sample of intermediate-mass black holes. We have performed analysis of multi-wavelength HST WFC3 and ACS/WFC data for several projects in the past and also utilized spectral and imaging data from all the top-20 largest ground-based optical telescopes.Supermassive Black Holes and Active GalaxiesGalaxies6falsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000GALAXYDWARF COMPACTNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000GALAXYDWARF COMPACTNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000GALAXYDWARF COMPACTNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1589WFC3/UVISImagingNoNoF300XWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF850LPWFC3/UVISImagingNoNoF300XWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF850LPWFC3/UVISImagingNoNoF300XWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF850LPWFC3/UVISImagingNoNoF300XWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF850LPPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX2falseThe scheduling data was generated by CASM 34.1.CASM was run in Phase II mode./private/var/folders/35/spdt8sqd3nq6406_62fcysx80000gn/T/OPVisit2406547137401033420.xml(Tic-Visit
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:pcs-time 380
:si-vis-utilization 2596
:al-overhead-at-end 77
:internal-dur-at-end 508
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2977
:pcs-gap 0
)true20