0 ----- Attempting Submission 2 (Fri Oct 05 19:51:15 GMT 2018) ----- ----- Attempting Submission 4 (Thu Dec 13 20:44:24 GMT 2018) ----- Testing Mid-Infrared AGN Selection in Dwarf Galaxies with Chandra and HST Studies of massive black holes (BH) in nearby dwarf galaxies can provide important constraints on the birth and growth of the first seed BHs in the early Universe. We propose joint Chandra and HST observations of 7 dwarf galaxies from our recent sample of mid-IR selected candidate AGNs in galaxies with stellar masses comparable to the Magellanic Clouds (Hainline et al. 2016). The proposed observations will enable us to firmly establish the presence of massive BHs in these dwarf galaxies, characterize the compact X-ray emission from the AGNs, and determine the properties of the host galaxies. Our results will also be compared to existing Chandra and HST observations of optically-selected AGNs in dwarfs that lack mid-IR signatures of an AGN. We propose HST Wide Field Camera 3 (WFC3) observations in three filters spanning a wavelength range of ~0.3 - 1.2um (UVIS F336W & F606W and IR F140W, corresponding to U-band, Wide V -band and Wide JH-band, respectively). The short wavelength observations will enable us to pinpoint the location of star-forming regions in our target galaxies with respect to the X-ray emission from an AGN and help correct for any contribution from X-ray binaries. We will also use spatially-resolved color diagnostics to investigate the ages of stellar populations in these dwarfs hosting mid-IR selected AGNs. The near-IR observations will enable us to determine the detailed morphologies and structural components of the galaxies with sufficient resolution and sensitivity to detect small, faint bulges. As shown below, we can achieve our science goals with one HST orbit per galaxy for a total of 7 orbits. We will use the IR/F140W filter to study the structures of our target galaxies. Based on surface brightness profiles of our faintest targets, we wish to reach a 10-sigma surface-brightness sensitivity of u_r ~ 23 mag arcsec^2 in a given pixel. Prior experience suggests that we will be able to reach at least a magnitude deeper with radial averaging than our per-pixel depth. This will allow us to detect the outer parts of the disks in our target galaxies, which is necessary to adequately decouple bulge and disk components on small scales. According to the WFC3/IR exposure time calculator, we need ~400 s to reach our required sensitivity in F140W. We will break the total time into 4 dithered exposures to improve the PSF sampling and avoid bad pixels. We will use the timing sequence STEP25 with NSAMP=9 (~100 s per exposure) to increase our dynamic range, avoid potential saturation from AGN, and allow the use of the IRSUB512 subarray to avoid buffer dumps. Our galaxies are quite compact so using a subarray will not compromise our science or limit our sky subtraction. We will also use two optical filters, UVIS F336W and F606W, to obtain important color diagnostics of the stellar populations and evolutionary state of our target dwarf galaxies. To ensure we can accurately separate bulge and disk components, we aim to reach a 10-sigma surface- brightness sensitivity of u_r ~ 23 mag arcsec^2 in a 7 x 7 pixel box (roughly equivalent to 2 x 2 IR pixels). The WFC3/UVIS exposure time calculator suggests we need ~ 750 s in F336W and ~ 600 s in F606W, assuming a young B star spectrum. We will break the total time into 3 dithered exposures and use the 1k x 1k subarray with chip 2. To summarize, we can achieve our science goals with 1 orbit per galaxy assuming a visibility of ~53 min. We will spend a minimum of ~400 s in F110W, ~600 s in F606W and ~750 s in F336W, leaving sufficient time for acquisition and instrument overheads (approximately 6 min for guide-star acquisition, 2 min for dithering, 14 min for readout, 1 min to switch from UVIS to IR). 6 false false false false false false false SUPPORTED GALAXY SEYFERT YES J2000 GALAXY SEYFERT YES J2000 GALAXY SEYFERT YES J2000 GALAXY STARBURST YES J2000 GALAXY STARBURST YES J2000 GALAXY STARBURST J2000 GALAXY STARBURST YES J2000 POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 1 false POS-TARG DITHER 0.572 LINE 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 2 false The scheduling data was generated by CASM 26.2.2. CASM was run in Phase II mode. /Users/amyreines/Proposals/HST/cycle25_midIR_dwarfs/phaseII-3point/OP-cache/revised2-v01.xml (Tic-Visit :proposal-id 15607 :visit-id "01" :proposal-version -1 :trans-version "20181130" :date "13-Dec-2018 13:32:34.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 288720 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15607 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15607 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2904 :al-overhead-at-end 0 :internal-dur-at-end 397 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3238 :pcs-gap 0 ) true 1 0 The scheduling data was generated by CASM 26.2.2. 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CASM was run in Phase II mode. /Users/amyreines/Proposals/HST/cycle25_midIR_dwarfs/phaseII-3point/OP-cache/revised2-v04.xml (Tic-Visit :proposal-id 15607 :visit-id "04" :proposal-version -1 :trans-version "20181130" :date "13-Dec-2018 13:36:36.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 288720 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15607 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15607 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2808 :al-overhead-at-end 0 :internal-dur-at-end 397 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0 The scheduling data was generated by CASM 26.2.2. 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