adsabs/AstroCLIMB huggingface dataset:
Paper: First Data Release of the Merian Survey: A Wide-field Imaging Survey of Dwarf Galaxies at z ∼ 0.06–0.10
Authors: Shany Danieli, Erin Kado-Fong, Song Huang, Yifei Luo, Ting S Li, Lee S Kelvin, Alexie Leauthaud, Jenny E. Greene, Abby Mintz, Xiaojing Lin, Jiaxuan Li, Vivienne Baldassare, Arka Banerjee, Joy Bhattacharyya, Diana Blanco, Alyson Brooks, Zheng Cai, Xinjun Chen, Akaxia Cruz, Robel Geda, Runquan Guan, Sean Johnson, Arun Kannawadi, Stacy Y. Kim, Mingyu Li, Robert Lupton, Charlie Mace, Gustavo E. Medina, Yue Pan, Annika H. G. Peter, Justin I. Read, Rodrigo Córdova Rosado, Allen Seifert, Erik J. Wasleske, Joseph Wick
Figure caption: Postage stamps of 12 dwarf galaxies from the Merian catalog are shown in the seven leftmost columns, corresponding to g, N540, r, N708, i, z, and y filters. Each galaxy has a spectroscopic redshift, obtained from either existing surveys (SDSS and GAMA) or new observations using Magellan/IMACS and Keck/DEIMOS (Section 3.3). The two rightmost columns show the continuum-subtracted Hα and [O III] maps, derived from N708 and N540, with the continuum estimated via a geometric average of the adjacent broad-band filter fluxes.
Paper: First Data Release of the Merian Survey: A Wide-field Imaging Survey of Dwarf Galaxies at z ∼ 0.06–0.10
Authors: Shany Danieli, Erin Kado-Fong, Song Huang, Yifei Luo, Ting S Li, Lee S Kelvin, Alexie Leauthaud, Jenny E. Greene, Abby Mintz, Xiaojing Lin, Jiaxuan Li, Vivienne Baldassare, Arka Banerjee, Joy Bhattacharyya, Diana Blanco, Alyson Brooks, Zheng Cai, Xinjun Chen, Akaxia Cruz, Robel Geda, Runquan Guan, Sean Johnson, Arun Kannawadi, Stacy Y. Kim, Mingyu Li, Robert Lupton, Charlie Mace, Gustavo E. Medina, Yue Pan, Annika H. G. Peter, Justin I. Read, Rodrigo Córdova Rosado, Allen Seifert, Erik J. Wasleske, Joseph Wick
Figure caption: Example dwarf galaxy (﹩\mathrm{log}({M}_{\star }/{M}_{\odot })=7.87﹩) from Merian DR1. The main panel shows the galaxy’s seven-band photometry (gray symbols) and the GAMA spectrum (black). The top panels (grayscale) show the HSC and Merian cutouts and the bottom right panels show the Hα and [O III] maps generated using the method described in A. Mintz et al. (2024).
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Spectral energy distributions with ∼2000 data points for ﹩\mathrm{log}\,Z/{Z}_{\odot }\,=﹩ 0.0, −0.4, −2.0 assuming a light BH seeding channel so that ﹩\mathrm{log}\,{M}_{\mathrm{BH}}/{M}_{\odot }=5.89,4.59,2.0﹩ for each metallicity, respectively. The model with fAGN = 0% has a poststarburst age of 25.1 Myr (maximum ULX contribution relative to stars), and the model with fAGN = 100% has a poststarburst age of 1 Myr (no ULX contribution).
Paper: First Data Release of the Merian Survey: A Wide-field Imaging Survey of Dwarf Galaxies at z ∼ 0.06–0.10
Authors: Shany Danieli, Erin Kado-Fong, Song Huang, Yifei Luo, Ting S Li, Lee S Kelvin, Alexie Leauthaud, Jenny E. Greene, Abby Mintz, Xiaojing Lin, Jiaxuan Li, Vivienne Baldassare, Arka Banerjee, Joy Bhattacharyya, Diana Blanco, Alyson Brooks, Zheng Cai, Xinjun Chen, Akaxia Cruz, Robel Geda, Runquan Guan, Sean Johnson, Arun Kannawadi, Stacy Y. Kim, Mingyu Li, Robert Lupton, Charlie Mace, Gustavo E. Medina, Yue Pan, Annika H. G. Peter, Justin I. Read, Rodrigo Córdova Rosado, Allen Seifert, Erik J. Wasleske, Joseph Wick
Figure caption: The flux distribution of sky objects in the N540 and N708 bands. The N708_gaap1p0Flux and N540_gaap1p0Flux fluxes are used. We show the patch-level and tract-level median (left) for sky objects in a representative tract (tract 8525) and a larger set of tracts, respectively, along with their corresponding median absolute deviation (MAD, right). The black bars represent the range from the 16th to 84th percentiles, and the white dots indicate the 50th percentile. These test results indicate good sky subtraction quality, with flux values for the sky objects remaining close to zero in both bands.
Paper: First Data Release of the Merian Survey: A Wide-field Imaging Survey of Dwarf Galaxies at z ∼ 0.06–0.10
Authors: Shany Danieli, Erin Kado-Fong, Song Huang, Yifei Luo, Ting S Li, Lee S Kelvin, Alexie Leauthaud, Jenny E. Greene, Abby Mintz, Xiaojing Lin, Jiaxuan Li, Vivienne Baldassare, Arka Banerjee, Joy Bhattacharyya, Diana Blanco, Alyson Brooks, Zheng Cai, Xinjun Chen, Akaxia Cruz, Robel Geda, Runquan Guan, Sean Johnson, Arun Kannawadi, Stacy Y. Kim, Mingyu Li, Robert Lupton, Charlie Mace, Gustavo E. Medina, Yue Pan, Annika H. G. Peter, Justin I. Read, Rodrigo Córdova Rosado, Allen Seifert, Erik J. Wasleske, Joseph Wick
Figure caption: Number counts of objects in the Merian-Wide DR1 photometric catalog (SciUse=1) as a function of the total mN708 magnitude, without any correction for incompleteness. The total number counts with no teff cuts is shown in black with Poisson errors. The brown and orange histograms show objects with teff > 0.5 tobs and teff > 0.9 tobs, respectively, where ﹩{t}_{\mathrm{obs}}=600\,{\rm{s}}﹩ for the N708-band.
Paper: First Data Release of the Merian Survey: A Wide-field Imaging Survey of Dwarf Galaxies at z ∼ 0.06–0.10
Authors: Shany Danieli, Erin Kado-Fong, Song Huang, Yifei Luo, Ting S Li, Lee S Kelvin, Alexie Leauthaud, Jenny E. Greene, Abby Mintz, Xiaojing Lin, Jiaxuan Li, Vivienne Baldassare, Arka Banerjee, Joy Bhattacharyya, Diana Blanco, Alyson Brooks, Zheng Cai, Xinjun Chen, Akaxia Cruz, Robel Geda, Runquan Guan, Sean Johnson, Arun Kannawadi, Stacy Y. Kim, Mingyu Li, Robert Lupton, Charlie Mace, Gustavo E. Medina, Yue Pan, Annika H. G. Peter, Justin I. Read, Rodrigo Córdova Rosado, Allen Seifert, Erik J. Wasleske, Joseph Wick
Figure caption: Example object detections (left) and their corresponding entries for a selection of catalog columns (right).
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Emission-line ratio sensitivity to Z (bottom axis) and MBH (top axis) for several common UV AGN diagnostics assuming a 1 Myr poststarburst age (no ULX contribution). The emission-line predictions are provided for the light seeding channel relative to a fiducial model assuming MBH = 105M⊙. The heavy, moderate, and light seeds reach an MBH floor at log MBH/M⊙ = 5.0, 3.5, and 2.0, respectively. The gray boxes represent regions where different seed mechanisms start to take effect. Except for [Ne V]/[Ne III], most of the line ratios in the UV are insensitive to MBH and IMBH seeding channels.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Sensitivity to Z and MBH for several common mid-IR emission-line ratio AGN diagnostics in the same manner as those from Figure 6 assuming a 1 Myr poststarburst age (no ULX contribution). IR emission-line ratios are more sensitive than both UV and optical emission-line ratios with [S IV] λ10.5 μm, [Ne II] λ12.8 μm, and [Ar II] λ6.99 μm showing the greatest sensitivity. Each subplot that contains one or more of these wavelengths shows a maximum difference of ≳0.8 dex.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: The luminosities of potential AGN diagnostics in the UV relative to Hα assuming a poststarburst age of 1 Myr (i.e., no ULX contribution).
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Spectral energy distributions for four distinct poststarburst ages (5.01–25.1 Myr) at various metallicities (﹩\mathrm{log}\,Z/{{\rm{Z}}}_{\odot }=﹩  0.0, −0.4, −2.0) and fAGN = 0% and 4% assuming a light BH seeding channel. The purple dashed line indicates the maximum ULX contribution (poststarburst age = 25.1 Myr and fAGN = 0%).
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Sensitivity to Z and MBH for several common optical emission-line ratio AGN diagnostics in the same manner as those from Figure 6. Emission-line ratios that contain He II λ4686, [O I] λ6300, and [S II] λ6720 show the greatest sensitivity, which makes them suitable candidates for constraining MBH and seeding channels.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: The difference between Te at the face of the cloud for the light seeding model and the fiducial model with MBH = 105M⊙. The variations in MBH associated with the light seeding model introduce differences in Te on the order of the emission-line excitation energies in the mid-IR.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Each panel shows multiple SEDs with different poststarburst ages of 1.0, 5.01, 10.0, and 25.1 Myr. The left panel has a metallicity set at ﹩\mathrm{log}\,Z/{Z}_{\odot }=﹩  −2. The right panel has a metallicity of ﹩\mathrm{log}\,Z/{Z}_{\odot }=﹩  −0.4. The AGN contributes 16% to the total ionizing flux, as denoted by fAGN = 16%, and assumes a light BH seeding channel. Both panels have vertical gray lines that represent relevant ionization potentials of different elements, as indicated by the labels above the graph, such as S II, C II, O II, etc.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: The line luminosities of potential AGN diagnostics in the IR relative to Hα assuming a poststarburst age of 1 Myr (i.e., no ULX contribution). Line styles and colors are the same as Figure 10.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: The line luminosities of potential AGN diagnostics in the optical relative to Hα assuming a poststarburst age of 1 Myr (i.e., no ULX contribution). Line styles and colors are the same as Figure 10.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Fraction of models correctly classified as AGN with several optical diagnostic diagrams (demarcations given in Table 2) in the same manner as Figure 15. The black dashed line is shown on the subplots with diagnostic diagrams that contain a composite or LINER zone (a), (b), (c), and (i). The area contained within this line is the maximum parameter space covered when not including the composite zone for these four diagnostic diagrams. The figure shows the Ne V diagram (panel (i)), can distinguish AGN models for fAGN; however, they all fall into the composite region (Figure 17). While many diagnostics can identify AGN in the metallicity range ﹩-0.8\,\leqslant \,\mathrm{log}\,Z/{Z}_{\odot }\,\leqslant \,﹩−0.2, they are susceptible to ULX contributions (red area).
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Fraction of models correctly classified as AGN with several UV diagnostic diagrams with varying physical parameters. We vary both fAGN and Z to calculate the fraction of models that are classified as AGN as indicated by the color bar. Each subplot uses a different diagnostic diagram to identify AGN with demarcations given in Table 1. The subplots are titled by the ionization parameter range in which they are likely to be observed as well as the age < 5 Myr at which the diagnostic diagram can categorize AGN models as AGN across the largest area of the fAGN–Z parameter space. The red area indicates where each diagram would distinguish AGN at an age ≥ 5 Myr, representing false-positive detection of an AGN due to a ULXs. The diagrams featuring C IV λλ1548,51 have the potential to identify dwarf AGN over a wide range of Z, down to low fAGN, but ULXs can mimic the presence of AGN.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Fraction of models correctly classified as AGN with mid-IR diagnostic diagrams (demarcations given in Table 3) in the same manner as Figure 16. All three diagrams can identify dwarf AGN over a 2 dex metallicity range with fAGN  ≥ 0.02.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: UV diagnostic diagrams capable of cleanly separating excitation from active IMBHs and starlight. The BPASS+ULX grid is capable of mimicking dwarf AGN emission to a significant degree, which strongly hinders the ability to robustly identify dwarf AGN in the UV.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Optical diagnostic diagrams using [O I] λ6300 show promise in separating active IMBHs and starlight excitation while minimizing ULX contributions. Unlike UV diagnostics, the BPASS+ULX model grids do not overlap with the AGN grids in either diagram for fAGN  ≳  0.16, which defines each diagram’s “AGN Threshold” demarcations. Together, the diagrams enable the identification of dwarf AGN spanning log Z/Z⊙ = −2.0 to log Z/Z⊙ = 0.0.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: The ratio of emission-line predictions assuming a poststarburst age of 25.1 Myr (i.e., maximum relative ULX contribution) to predictions assuming a poststarburst age of 1 Myr (i.e., no ULX contribution) with a light seeding channel for select AGN diagnostics in the UV-IR. The gold band represents when ULX contribution dips below 10%. The level of ULX contribution as a function of fAGN depends upon U and Z, without any noticeable trends according to wavelength band. Colors and line styles are in the same format as Figure 10.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: The effectiveness of the [Ne V]/[Ne III] diagnostic diagram from Figure 16 regenerated without including the composite region of that diagram. Most AGN models reside in the composite region, rendering the diagram relatively ineffective at identifying the majority dwarf AGN.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Optical diagnostic diagrams that show promise in separating active IMBHs and starlight excitation while minimizing ULX contributions. Unlike UV diagnostics, the BPASS+ULX model grids have no overlap with the AGN grids in the He II diagram for fAGN ≳ 0.04 and no overlap with the AGN grids in the [Ne III] diagram for fAGN ≳ 0.16. These limits are defined as “AGN Threshold” demarcations in each diagram.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: The predicted broadband (2–10 keV) fluxes assuming a heavy seeding channel (top) and a light seeding channel (bottom), relative to a fAGN   =  0 model. The dashed black line represents when the IMBH contribution dominates over the ULX contribution by a factor of five . The light seeding model strongly enhances LX in the lowest-metallicity simulations.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: Mid-IR diagnostic diagrams showing the most promise in separating active IMBHs and starlight excitation while minimizing possible ULX contributions. The models shown represent excitation due to stars (cyan), stars+ULX (blue), stars+AGN (orange), stars+ULX+AGN (red), and shocks (green). Unlike the UV and optical diagnostics, the [O IV]/[Ne III] vs. [S IV]/[Ne II] and [O IV]/[S III] vs. [S IV]/[Ar II] diagrams show a relatively clean distinction between excitation due to stars, ULXs, AGN, and shocks.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: A subset of our models with low and high AGN accretion rates. The [O IV]/[S III] vs. [S IV]/[Ar II] diagram remains valuable for separating excitation from active IMBHs and stars.
Paper: Emission-line Diagnostics for IMBHs in Dwarf Galaxies: Accounting for Black Hole Seeding and Ultraluminous X-Ray Source Excitation
Authors: Chris T. Richardson, Jordan Wels, Kristen Garofali, Julianna M. Levanti, Vianney Lebouteiller, Bret Lehmer, Antara Basu-Zych, Danielle Berg, Jillian M. Bellovary, John Chisholm, Sheila J. Kannappan, Erini Lambrides, Mugdha S. Polimera, Lise Ramambason, Maxime Varese, Thomas Vivona
Figure caption: A subset of our models with a higher gas density of log nH = 4.0 compared to our standard model that uses log nH = 2.0. The [O IV]/[S III] vs. [S IV]/[Ar II] diagram shows almost all of the AGN models residing in the AGN region.
Paper: A Pseudo-Newtonian Stationary Circumbinary Slim Disk Model
Authors: Sixiang Wen, Vasileios Paschalidis
Figure caption: Slim disk results vs. thin disk results. Top panel (left to right column): viscous torque Tϕr, radiative flux Qrad, surface density, and H/r profiles for the different disk models. Magenta lines and cyan lines denote the thin disk results for cases of Tϕr = −3νΣΩk/2 and Tϕr = −αP, respectively, while the blue lines show the slim disk results. The color dotted lines denote q = 0, while the color solid lines represent q = 10−3 for cases of both slim and thin disks. The disk parameters are ﹩\dot{m}=0.1﹩, Mp = 108M⊙, and a = 100Rg for all the three models.