adsabs/AstroCLIMB huggingface dataset:
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Model parameters in basic NICER spectral fitting. Left: T in vs. the unabsorbed rest-frame 0.3–2  keV luminosity in the diskbb component. Middle: equivalent width of the 1 keV line vs. L 0.3−2,unabs, only plotted for observations where the model fit with the Gaussian component is favored with the BIC criterion. Right: σ line of 1 keV line vs. L 0.3–2,unabs.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Spectral modeling results of the NICER observation on MJD 59905.498—the one with the highest χ 2/dof in the initial analysis. From left to right, we show the data, best-fit models, and residuals under four different models. Models (c) and (d) give acceptable fits.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: NICER observed 0.3–2 keV light curve of AT2022lri at δ t < 254 days. The black asterisks mark four observations with high-quality data (E upper > 2.1 keV, net counts > 5 × 104) selected for an initial basic spectral modeling. The magenta cross mark one observation selected for detailed modeling (see Figure 12). The large circles mark the assigned indices of seven observations during one X-ray dip (see Figure 13).
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Seven observations around δ t ∼ 196 days jointly modeled with three different models. We show the data, best fits, and residuals for the fiducial continuum model (A) in the top two rows, the absorption+emission model (C) in the middle two rows (see Table 3 for the best-fit parameters), and the reflection model (D) in the bottom two rows (see Table 4 for the best-fit parameters).
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Ratio of the XMM E2 (left) and XMM E3 (right) EPIC/pn data fit to various models.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: A comparison between the RGS spectrum of AT2022lri to that of ASASSN-14li (J. M. Miller et al. 2015). While strong narrow absorption lines were seen in ASASSN-14li, the spectrum of AT2022lri can be well described by the continuum model.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: XMM-Newton/EPIC light curve of AT2022lri in the second (left) and third (right) epochs. Bins with background flaring have been masked out.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Atmospheric stratification and radiative losses inferred from the IBIS and IRIS spectra. In all panels, the blue and orange lines correspond to the IBIS and IBIS+IRIS fits, respectively. (a) Temperature (top) and LOS velocity (bottom) at the location marked by the circle in Figure 1; the error bars show the uncertainties in the chromosphere. (b) The foreground shows observed and best-fit intensities in the λ5896 (left) and λ8542 (right) lines, and the background shows normalized temperature response functions as a function of column mass and wavelength for the corresponding models shown in (a). (c) Analogous to (b) but for a wavelength window around the λ2796 line. (d) Histograms of integrated radiative losses in the low chromosphere for all IRIS slit positions.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Deposited acoustic flux vs. losses in the plage region. The left (right) column shows the results for the IBIS (IBIS+IRIS) inversions, separated for weakly (blue) and strongly (orange) magnetized regions. (a)–(c) Acoustic flux deposited between the formation heights of sodium, calcium, and magnesium. (d)–(f) The respective ratios of acoustic fluxes to the radiative losses.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Phase difference between the velocities in λ5896 and λ8542. The two-dimensional histogram of phase values (inverse color, arbitrary scaling) is obtained from the inversion models in the quiet patch as a function of frequency. The markers show the maximum value in each frequency bin. The solid white line shows a linear fit to the underlying points corresponding to the time delay, Δt.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Temperature and velocity oscillations in the quiet patch. (a) Power spectral densities of inverted LOS velocities and temperatures at the temperature minimum (dotted), the core of λ5896 (dashed), and the core of λ8542 (solid). (b) Temperature and mass density as a function of logarithmic column mass at a selected location shown by the white cross on the right panels; the three black markers show the column mass values of the temperature minimum (triangle), the core of λ5896 (square), and the core of λ8542 (circle). (c)–(e) Acoustic fluxes at the three considered heights. The white dots on the color bars indicate median values.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Lead–lag analysis of inverted temperature and velocity at two height ranges in the quiet patch. From left to right: cross-correlation coefficient, coherence, and lag between temperature and velocity at the formation height of λ5896 (top) and λ8542 (middle), and between velocities in the two lines at different heights (bottom). The white crosses show the three locations displayed in Figure 7.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Time variation of velocity, temperature, and total cooling rates in the low chromosphere in the quiet patch. From top to bottom: LOS velocities, windowed correlation lag (with correlation coefficients, r), temperature, and integrated radiative losses as a function of time for the pixel locations (A), (B), and (C) marked in Figures 5 and 6. The gray lines show (spatially) averaged quantities in the FOV.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Radiative losses and deposited acoustic flux in the low chromosphere. (a) Time-averaged, deconvolved HMI LOS magnetogram; the range is capped at ±100 G for display purposes. (b) Time-averaged radiative losses in the low chromosphere. (c) Ratio between the deposited acoustic flux and the radiative losses. The crosses show the three locations displayed in Figure 7. The white dots on the color bars show median values.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Inversions of the quiet patch. (a), (b) Observed intensities in the core of λ5896 and λ8542. (c), (d) Corresponding synthetic intensities. (e) Example observed spectra (dots) and best fit (lines) at the two locations marked in the left panels.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Photospheric magnetic field and radiative losses in the chromosphere. Top panels: closest-in-time Hinode LOS magnetogram (a) and inclination angle (b) corresponding to the IRIS/IBIS time series; dotted lines indicate the IRIS slit positions. Bottom panels: Radiative losses vs. total field strength (c) and inclination angle (d) for the IBIS (blue) and IBIS+IRIS (orange) inversions.
Paper: Double-peaked Narrow Emission-line Galaxies in SDSS-IV MaNGA
Authors: Jiajie Qiu, Shiyin Shen, Shuai Feng, Yanmei Chen, Ruixiang Chang, Qianwen Zhao, Qi Zeng
Figure caption: The color-coded distributions of the DPG parameters of the DPSs on the Δv–r/R  e  plane, which have been smoothed by the LOESS algorithm. The DPG parameters include M * (top left), sSFR (top right), Sérsic index n (bottom left), and KA (bottom right). The number density of DPSs in the Δv–r/R  e  plane is shown as the contours in each panel (the same as the bottom right panel of Figure 4). Three types (the inner low-Δv, inner high-Δv, and outer DPSs) are divided by the dotted lines according to r/R  e  = 0.75 and Δv/(km s−1) = 300.
Paper: Double-peaked Narrow Emission-line Galaxies in SDSS-IV MaNGA
Authors: Jiajie Qiu, Shiyin Shen, Shuai Feng, Yanmei Chen, Ruixiang Chang, Qianwen Zhao, Qi Zeng
Figure caption: Top left: the SNR (>5) distributions of 5420 DPSs (red) and all other normal spaxels (black). Top right: distributions of r/R  e  of all DPSs (red), normal spaxels (black), and SNR-matched normal spaxels (blue). Their average values are marked with dotted lines with the corresponding colors. Bottom left: distributions of Δv of DPSs, fitted by a Gaussian profile (dotted line). Bottom right: the DPSs in the Δv–r/R  e  plane. Contours are plotted by their number density with peaks marked by black triangles.
Paper: Double-peaked Narrow Emission-line Galaxies in SDSS-IV MaNGA
Authors: Jiajie Qiu, Shiyin Shen, Shuai Feng, Yanmei Chen, Ruixiang Chang, Qianwen Zhao, Qi Zeng
Figure caption: Two examples (MaNGA ID 1-244377 and 1-604912) of DPGs with different types of DPSs. The left panels shows their optical images with morphological features. The middle panels show the 2D distributions of different DPSs in the same fields as the left ones (green: the inner low-Δv DPSs; red: the inner high-Δv DPSs; blue: the outer DPSs). The right panels give the 2D distributions of different DPSs in the Δv–r/R  e  plane. MaNGA ID 1-244377 with a bar, an AGN, and tidal feature has all three types of DPSs. MaNGA ID 1-604912 is an AGN-hosting galaxy but we only found inner low-Δv DPSs at center.
Paper: Double-peaked Narrow Emission-line Galaxies in SDSS-IV MaNGA
Authors: Jiajie Qiu, Shiyin Shen, Shuai Feng, Yanmei Chen, Ruixiang Chang, Qianwen Zhao, Qi Zeng
Figure caption: Similar plots as Figure 8 but for physical features, including bars (top left), AGNs (top right) and tidal features (bottom left).
Paper: Double-peaked Narrow Emission-line Galaxies in SDSS-IV MaNGA
Authors: Jiajie Qiu, Shiyin Shen, Shuai Feng, Yanmei Chen, Ruixiang Chang, Qianwen Zhao, Qi Zeng
Figure caption: Three instances of paired galaxies exhibiting DPSs. In each galaxy, the location of the DPSs is roughly represented by a white rectangle. MaNGA ID 1-251269 (left) represents a merging system with prominent tidal features. MaNGA 1-585230 (middle) lacks distinct tidal features, yet the DPSs are positioned outside the overlapping area of the galaxy pair. MaNGA 1-278185 (right) displays a pair of galaxies without any tidal features, with DPSs located in the intersecting area of the two galaxies.
Paper: Double-peaked Narrow Emission-line Galaxies in SDSS-IV MaNGA
Authors: Jiajie Qiu, Shiyin Shen, Shuai Feng, Yanmei Chen, Ruixiang Chang, Qianwen Zhao, Qi Zeng
Figure caption: The distributions of global properties of DPGs (red) and the control sample of normal galaxies (blue), including M halo (top left), Sérsic index n (top right), sSFR (bottom left), and KA (bottom right).
Paper: Double-peaked Narrow Emission-line Galaxies in SDSS-IV MaNGA
Authors: Jiajie Qiu, Shiyin Shen, Shuai Feng, Yanmei Chen, Ruixiang Chang, Qianwen Zhao, Qi Zeng
Figure caption: The distributions of M * of all MaNGA galaxies (black histograms), DPGs (red), and the control sample of normal galaxies (blue). The mean values of the physical parameters are marked as vertical dotted lines in the same color as the histograms.
Paper: Double-peaked Narrow Emission-line Galaxies in SDSS-IV MaNGA
Authors: Jiajie Qiu, Shiyin Shen, Shuai Feng, Yanmei Chen, Ruixiang Chang, Qianwen Zhao, Qi Zeng
Figure caption: The distributions of physical features of DPGs (red) and the control sample of normal galaxies (blue), including bars, AGNs, and tidal features, labeled as F(Bar), F(AGN), and F(Tidal), respectively.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Structures of very low-mass stars and brown dwarfs computed with the PARSEC code (A. Bressan et al. 2012), from the center to the atmosphere, in a stage close to the zero-age main sequence. The initial mass changes in increments of 0.05 M ⊙, from 0.05 M ⊙ to 0.7 M ⊙. The initial chemical composition is scaled solar according to E. Caffau et al. (2011), with a metallicity Z = 0.014, and helium abundance Y = 0.273. The horizontal line marks the maximum value, ﹩\mathrm{log}(R)=1﹩, currently available in the low-temperature Rosseland mean opacities (J. W. Ferguson et al. 2005; P. Marigo et al. 2022). Left panel: structures in the ﹩\mathrm{log}(T)-\mathrm{log}(R)﹩ plane, color coded according to the initial stellar mass. Right panel: structures in the ﹩\mathrm{log}(T)-\mathrm{log}(R)﹩ plane, with convective regions color coded according to the degree of superadiabaticity, ∇ − ∇ad. The gray sections correspond to convective regions treated as adiabatic, while the black sections refer to the radiative regions. See text for more details.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Left panel: the equation of state for a gas of free particles in the ﹩\mathrm{log}(T)-\mathrm{log}(\rho )﹩ plane. The dashed blue lines are approximate boundaries between regions where radiation pressure, classical ideal gas pressure, and nonrelativistic electron degeneracy dominate. We assume E. Magg et al. (2022)'s solar composition with X = 0.7 and Z = 0.01. The gray area denotes the upper extension of our opacity tables. The red and black lines mark the locus of points where the ionization degree of hydrogen is 0.5 and 0.2, as indicated. Right panel: ionization degree of hydrogen as a function of temperature for ﹩\mathrm{log}(R)=6﹩ (black line) and ﹩\mathrm{log}(R)=3﹩ (magenta line). In both panels, the plasma IPD effect is represented by solid lines, while dashed lines are the result of the classical Saha ionization equation. See text for more details.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Atmospheric pressure–temperature profiles for exoplanets, brown dwarfs, and very low-mass stars. The two hot Jupiter exoplanets, WASP-17b with a mass of 0.51 M J, and WASP-19b with a mass of 1.14 M J, were analyzed by D. K. Sing et al. (2016) through Hubble Space Telescope/Spitzer observations. E. Calamari et al. (2022) used an atmospheric retrieval analysis to derive the profile for the brown dwarf Gliese 229B with an estimated mass of 50 M J. We also add two theoretical profiles for brown dwarfs with a surface gravity of ﹩\mathrm{log}(g)=4.5﹩ (I. Baraffe et al. 2002), and a very low-mass star model from PARSEC (A. Bressan et al. 2012). The dashed black line denotes the limit below which pressure broadening for molecular spectral lines should be included. Refer to Section 3.2 for more details.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Distribution of several condensed species as a function of temperature at ﹩\mathrm{log}(R)=6﹩, for solar abundances in phase equilibrium, computed with GGchem. The abundances are evaluated with respect to the number density of hydrogen nuclei. The assumed ﹩\mathrm{log}(R)﹩ value and chemical composition are the same as in Figure 4.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Gaseous molecular concentrations, in number density, for some selected species as a function of temperature, without condensation. We assume ﹩\mathrm{log}(R)=6﹩, with a chemical composition solar-scaled according to E. Magg et al. (2022), with metallicity Z = 0.01 and hydrogen abundance X = 0.7.
Paper: The VIRUS-dE Survey. I. Stars in Dwarf Elliptical Galaxies—3D Dynamics and Radially Resolved Stellar Initial Mass Functions
Authors: Mathias Lipka, Jens Thomas, Roberto Saglia, Ralf Bender, Maximilian Fabricius, Gary J. Hill, Matthias Kluge, Martin Landriau, Ximena Mazzalay, Eva Noyola, Taniya Parikh, Jan Snigula
Figure caption: Basic Properties of the Galaxy Sample From left to right: the Virgo Cluster Catalog (VCC) identification number (B. Binggeli et al. 1985); the color identification used throughout this article; the morphological subclassification following T. Lisker et al. (2007; bc: blue center, di: disk feature, N: classical dE with nucleus, nN: classical dE without nucleus); the distance adopted from J. P. Blakeslee et al. (2009)—if there are no distances available (other than from redshifts), we use the average Virgo Cluster distance of 16.5 Mpc; the heliocentric velocity cz that we measured from the spectra; the projected distance to M87 (assuming d = 16.5 Mpc); the stellar mass we obtained; the photometric band we use for modeling of the light distribution; effective radius (in the z band), Sérsic index, and position angle all adopted from L. Ferrarese et al. (2006), who investigated all galaxies in our sample except for VC 308 (for which we consulted Hyperleda instead; D. Makarov et al. 2014). Note that VCC 308 and VCC 1861 appear almost perfectly round; therefore, a robust PA is not given.