adsabs/AstroCLIMB huggingface dataset:
Paper: VERTICO. IV. Environmental Effects on the Gas Distribution and Star Formation Efficiency of Virgo Cluster Spirals
Authors: Vicente Villanueva, Alberto D. Bolatto, Stuart Vogel, Tobias Brown, Christine D. Wilson, Nikki Zabel, Sara Ellison, Adam R. H. Stevens, María Jesús Jiménez Donaire, Kristine Spekkens, Mallory Tharp, Timothy A. Davis, Laura C. Parker, Ian D. Roberts, Dhruv Basra, Alessandro Boselli, Barbara Catinella, Aeree Chung, Luca Cortese, Bumhyun Lee, Adam Watts
Figure caption: Ratio of the integrated CO (2–1) line intensity in an annulus after stacking to that before stacking. The vertical black dashed line is the median value of log10[I CO,Stack/I CO,Unstack] = 0.21; this shows that, on average, stacking recovers ∼60% more emission. On average, we are reaching a characteristic rms noise of 0.1 mK at 10 km s−1, which corresponds to a sensitivity of ∼0.1 M ⊙ pc−2. The inset panel compares log10[I CO,Stack/I CO,Unstack] vs. galactocentric radius and shows that annuli with the most CO flux enhancement are at r ≳ 0.5r 25.
Paper: VERTICO. IV. Environmental Effects on the Gas Distribution and Star Formation Efficiency of Virgo Cluster Spirals
Authors: Vicente Villanueva, Alberto D. Bolatto, Stuart Vogel, Tobias Brown, Christine D. Wilson, Nikki Zabel, Sara Ellison, Adam R. H. Stevens, María Jesús Jiménez Donaire, Kristine Spekkens, Mallory Tharp, Timothy A. Davis, Laura C. Parker, Ian D. Roberts, Dhruv Basra, Alessandro Boselli, Barbara Catinella, Aeree Chung, Luca Cortese, Bumhyun Lee, Adam Watts
Figure caption: Spectral stacking example. The average CO (2–1) spectrum within an annulus that spans from 0.6r 25 to 0.7r 25 in NGC 4536 is shown. The left panel shows the average of all spectra in the annulus in the observed velocity frame. The inset panel includes the SDSS r-band image (background), CO (2–1) data (blue contours), and the annulus that spans from 0.6r 25 to 0.7r 25 (red ellipses). The right panel shows the average in the velocity frame relative to H I, along with the best Gaussian fit profile (green dashed line).
Paper: VERTICO. IV. Environmental Effects on the Gas Distribution and Star Formation Efficiency of Virgo Cluster Spirals
Authors: Vicente Villanueva, Alberto D. Bolatto, Stuart Vogel, Tobias Brown, Christine D. Wilson, Nikki Zabel, Sara Ellison, Adam R. H. Stevens, María Jesús Jiménez Donaire, Kristine Spekkens, Mallory Tharp, Timothy A. Davis, Laura C. Parker, Ian D. Roberts, Dhruv Basra, Alessandro Boselli, Barbara Catinella, Aeree Chung, Luca Cortese, Bumhyun Lee, Adam Watts
Figure caption: Distribution of offsets between the CO (2–1) and H I velocities, ΔV = V CO(2−1) − V HI, in spaxels within the 38 VERTICO galaxies analyzed here. The red bars correspond to spaxels with ΔV offsets that place CO outside the integration window (see text) for stacking CO. The vertical black dashed line is the median value of ΔV = −0.7 km s−1. The figure shows that, on average, the differences between the CO (2–1) and H I velocities are smaller than the integration window in most cases (∼98%).
Paper: Effects of Inner Halo Angular Momentum on the Peanut/X Shapes of Bars
Authors: Sandeep Kumar Kataria, Juntai Shen
Figure caption: This figure shows the visual overlay of circles, with radii representing bar lengths measured using various methods, on the contour plot of bar in S000 model. The methods includes ﹩\displaystyle \frac{{A}_{2}}{{A}_{0}}﹩ peak technique, a 5 and a 10 as mentioned in Figure 11, a min and a max mentioned in Figure 10.
Paper: Effects of Inner Halo Angular Momentum on the Peanut/X Shapes of Bars
Authors: Sandeep Kumar Kataria, Juntai Shen
Figure caption: Top panel shows the variation of ﹩\displaystyle \frac{{A}_{2}}{{A}_{0}}﹩ with radius; bottom panel shows the variation of the bar phase angle (ϕ) with radius. The solid line corresponds to radius at which ﹩\displaystyle \frac{{A}_{2}}{{A}_{0}}﹩ peaks; dotted–dashed line corresponds to radii at which bar phase angle (ϕ) deviates from constant value by 5° and 10° respectively.
Paper: Effects of Inner Halo Angular Momentum on the Peanut/X Shapes of Bars
Authors: Sandeep Kumar Kataria, Juntai Shen
Figure caption: This figure shows the bar strength time evolution for lowest- and highest-spin models. Solid line models are generated using GalIC initial condition generator while dashed line models are generated using Agama initial condition generators.
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: SFR enhancement as a function of projected separation of pairs. SFR enhancement is defined as the ratio of the weighted average of the SFR of the pair sample to that of the control sample (Equation (1)). The filled blue circles and filled red diamonds correspond to the SFR enhancement for the ΔV < 1000 km s−1 and ΔV < 5000 km s−1 pair samples, respectively. The dotted line corresponds to a value of one, which represents no interaction-induced SFR enhancement. We see the highest level of SFR enhancement at a factor of 1.23﹩{}_{-0.09}^{+0.08}﹩ (∼2.6σ) and ﹩{1.15}_{-0.04}^{+0.05}﹩ (∼3.0σ) in the closest separation bin with projected pair separation <25 kpc for galaxy pair sample with ΔV < 1000 km s−1 and ΔV < 5000 km s−1, respectively. We note that there is a significant amount of scatter around the SFR enhancement value of one.
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: SFR enhancement as a function of projected separation for the galaxy pairs with ΔV < 1000 km s−1 and with the stellar mass of the primary (more massive) galaxy M  p  less than 10.88 M ⊙ (left) and more than 10.88 M ⊙ (right) for the pair sample with ΔV < 1000 km s−1. The dotted line corresponds to a value of one, which represents no interaction-induced SFR enhancement.
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: Distribution of paired galaxies (red scatter points) and controls (contours) on the SFR–M * plane for (top to bottom) the 0.5 < z < 3.0, 0.5 < z < 1.0, 1.0 < z < 1.5, 1.5 < z < 2.0, and 2.0 < z < 3.0 bins. The black solid line in each subplot corresponds to the SFMS (Whitaker et al. 2014) in the given redshift range. The gray lines correspond to the SFR value above and below the SFMS by a factor of 3 in each redshift bin.
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: Normalized (at peak) distributions of environmental overdensity (left panel), spectroscopic redshift (middle panel), and stellar mass (right panel) of spectroscopic galaxy pairs (solid lines; with projected separation <150 kpc, mass ratio <4, and spectroscopic redshift between 0.5 and 3 for the ΔV < 5000 km s−1, top, and ΔV < 1000 km s−1, bottom, samples, respectively) and their corresponding mass-, redshift-, and environment-matched control galaxies (dashed black lines).
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: Comparison of the SFR (left) and stellar mass (right) measured using SED3FIT and MAGPHYS for galaxies in our sample with a large 8 μm residual suggesting the presence of an AGN component in the mid-IR (MIR). The color bar shows the value of the AGN fraction estimated using SED3FIT for a given galaxy.
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: Distribution of weights (w  i ) with respect to the SFR of galaxy pairs (SFR P ). The distribution shows that there is no significant trend between the weights and SFR P .
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: The decision tree for computing the combined SFR, SFR P , of a galaxy pair, where galaxy1 and galaxy2 correspond to the primary and secondary galaxies in a given galaxy pair, respectively.
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: SFR enhancement as a function of projected separation for the galaxy pairs with ΔV < 1000 km s−1 at z < 1 (left) and z > 1 (right). The dotted line corresponds to a value of one, which represents no interaction-induced SFR enhancement.
Paper: On the Triggering of Extreme Starburst Events in Low-metallicity Galaxies: A Deep Search for Companions of Green Peas
Authors: Lauren Laufman, Claudia Scarlata, Matthew Hayes, Evan Skillman
Figure caption: Star formation rates (SFRs) and stellar masses of the green peas in comparison to the control sample. The green peas are represented by green circles, with filled-in circles for those that have companions, and unfilled circles for those that do not. The masses used are from Izotov et al. (2011) when available, otherwise from Cardamone et al. (2009). The error bars on the SFRs are in lime green. The blue × shapes represent the control sample galaxies from 3D-HST. The filled-in × have companions, and the unfilled × do not. The red triangles are all of the galaxies from the 3D-HST catalog that have a spectroscopically confirmed redshift between 0.15 < z < 0.3. It is interesting that there are no control sample galaxies in the mass range >9.5; these types of galaxies exist in the 3D-HST survey, but they are not spatially located in the MUSE-Wide footprint.
Paper: On the Triggering of Extreme Starburst Events in Low-metallicity Galaxies: A Deep Search for Companions of Green Peas
Authors: Lauren Laufman, Claudia Scarlata, Matthew Hayes, Evan Skillman
Figure caption: Control sample galaxies plotted in the MUSE-Wide footprint. The gray circles are the control sample galaxies chosen from 3D-HST. Only the galaxies inside the dashed line are included, as the ones outside the dotted line could potentially have companions outside the MUSE-Wide footprint that would be missed. The orange symbols represent the control sample galaxies that have been identified as having companions, and the blue symbols represent the companion galaxies identified from MUSE-Wide. The two instances where the blue and orange overlap are actually the same pairing found twice (the pairs are not the symbols overlapping, but rather one from each). In other words, the the overlapping blue and orange symbols mean a galaxy was identified as both a galaxy in 3D-HST and a companion in MUSE-Wide.
Paper: On the Triggering of Extreme Starburst Events in Low-metallicity Galaxies: A Deep Search for Companions of Green Peas
Authors: Lauren Laufman, Claudia Scarlata, Matthew Hayes, Evan Skillman
Figure caption: Posterior probability distributions for the fraction of galaxies with at least one companion. Green and purple show green pea and control sample, respectively. In all distributions, the dark shaded regions are the 68% credible intervals, and the light shaded regions are the 95% credible intervals. In the left panel we show the results computed using the full MUSE area for all galaxies, while on the right we limit the companion search to the same physical area (a circle of 78 kpc radius) at all redshifts.
Paper: On the Triggering of Extreme Starburst Events in Low-metallicity Galaxies: A Deep Search for Companions of Green Peas
Authors: Lauren Laufman, Claudia Scarlata, Matthew Hayes, Evan Skillman
Figure caption: Left column: SDSS images of the green peas (J094458, J124834, J163719, J161306) and their companions. In the SDSS images, two of the four companions are not visible. Middle column: spectra of the aforementioned green peas. Right column: spectra of the companions of the aforementioned galaxies. The plotted wavelengths are in the observed frame. Companion galaxies have fainter continua compared to the main green pea galaxy, and residual flux from the sky subtraction process is more prominent in their spectra. The main emission-line features detected in each spectrum are labeled.
Paper: On the Triggering of Extreme Starburst Events in Low-metallicity Galaxies: A Deep Search for Companions of Green Peas
Authors: Lauren Laufman, Claudia Scarlata, Matthew Hayes, Evan Skillman
Figure caption: Example of a background absorption galaxy put through the code to match with a template absorption spectrum and determine the redshift. The template spectrum used is the elliptical galaxy from the Kinney–Calzetti Atlas in pysynphot. The upper figure is the χ 2 per degree of freedom for each redshift that the template was shifted to and compared to the object’s observed spectrum. The red vertical line is the redshift where the χ 2 is the lowest. The lower figure has the observed spectrum in blue, the shifted template in orange, and the uncertainty on the data in green.
Paper: On the Triggering of Extreme Starburst Events in Low-metallicity Galaxies: A Deep Search for Companions of Green Peas
Authors: Lauren Laufman, Claudia Scarlata, Matthew Hayes, Evan Skillman
Figure caption: Method of subtracting a continuum image from a narrowband image to capture everything emitting specifically at that wavelength. The left image displays the pseudo-narrowband Hα image for J161306, the middle image contains the pseudo-narrowband continuum, and the right image is the difference between the two. The green pea and its companion are clearly visible. The x and y axes are in pixels.
Paper: On the Triggering of Extreme Starburst Events in Low-metallicity Galaxies: A Deep Search for Companions of Green Peas
Authors: Lauren Laufman, Claudia Scarlata, Matthew Hayes, Evan Skillman
Figure caption: Comparison of Hα luminosity of the green peas and companions with the 5σ Hα line luminosity limit for each green pea field. The secondary y-axis is the SFR, assuming Bell & Kennicutt (2001). The green peas are represented by green circles, the companions are represented by orange diamonds, and the Hα line luminosity limits are represented by blue triangles. The luminosities of the companions are well above all the line luminosity limits.
Paper: The σHβ -based Dimensionless Accretion Rate and Its Connection with the Corona for AGNs
Authors: Yu-Qin Chen, 玉琴 陈, Yan-Sheng Liu, 延盛 刘, Wei-Hao Bian, 维豪 卞
Figure caption: Left: F X vs. ﹩\dot{M}﹩. The green circles denote Swift/BAT-detected AGNs, and the gray circles denote SDSS AGNs. Red squares represent 32 RM sources in our sample. Blue circles denote 8 AGNs with stellar velocity dispersions. The solid black line is our best fit. The vertical dashed line is ﹩\dot{M}﹩ = 3. Right: dependence of F X on ﹩\dot{M}﹩ and M BH. The solid line is 1:1.
Paper: The σHβ -based Dimensionless Accretion Rate and Its Connection with the Corona for AGNs
Authors: Yu-Qin Chen, 玉琴 陈, Yan-Sheng Liu, 延盛 刘, Wei-Hao Bian, 维豪 卞
Figure caption: The relation between ﹩2\mathrm{log}({\sigma }_{{\rm{H}}\beta }/{\mathrm{FWHM}}_{{\rm{H}}\beta })+\mathrm{log}5.5﹩ and FWHMHβ , i.e., f vs. FWHMHβ . The black solid line is our best fit with a slope of −0.61. The red dashed line is the result of Yu et al. (2020b) with a slope of −1.1. The two vertical dashed lines denote 2000 and 4000 km s−1. The blue squares denote AGNs from Wang et al. (2019a), and the green triangles denote AGNs from Huang et al. (2022).
Paper: The σHβ -based Dimensionless Accretion Rate and Its Connection with the Corona for AGNs
Authors: Yu-Qin Chen, 玉琴 陈, Yan-Sheng Liu, 延盛 刘, Wei-Hao Bian, 维豪 卞
Figure caption:  L Bol/L Edd vs. ﹩\dot{M}﹩. Red squares represent 32 RM sources in our sample. Blue circles denote 8 AGNs with stellar velocity dispersion. The solid line is our best fit showing a nonlinear relation, ﹩{L}_{\mathrm{Bol}}/{L}_{\mathrm{Edd}}\propto {\dot{M}}^{0.56}﹩. The dashed−dotted line is the relation assuming a constant coefficient of η = 0.1. The dashed line is ﹩\dot{M}﹩ = 3, which is the criterion distinguishing super-Eddington SMBHs and sub-Eddington SMBHs.
Paper: The σHβ -based Dimensionless Accretion Rate and Its Connection with the Corona for AGNs
Authors: Yu-Qin Chen, 玉琴 陈, Yan-Sheng Liu, 延盛 刘, Wei-Hao Bian, 维豪 卞
Figure caption: An example of optical spectral decomposition. The pseudo-continuum including the host galaxy, Fe II, a power law, and a third-order polynomial is shown, as well as the narrow and broad profiles for Hβ, He II, [O III], Hα, [N II], and [S II]. The bottom panels show the line fitting around Hβ (left) and Hα (right).
Paper: The σHβ -based Dimensionless Accretion Rate and Its Connection with the Corona for AGNs
Authors: Yu-Qin Chen, 玉琴 陈, Yan-Sheng Liu, 延盛 刘, Wei-Hao Bian, 维豪 卞
Figure caption: Γ of AGNs with BAT data vs. Γ of AGNs without BAT data for a sample by Liu et al. (2021). The dashed red line is 1:1. The solid line is the best linear fit with a fixed slope of 1. The inset in the lower right corner shows the distribution of their differences.
Paper: The σHβ -based Dimensionless Accretion Rate and Its Connection with the Corona for AGNs
Authors: Yu-Qin Chen, 玉琴 陈, Yan-Sheng Liu, 延盛 刘, Wei-Hao Bian, 维豪 卞
Figure caption: The 5100 Å luminosity L 5100 vs. redshift z. The blue circles denote AGNs from Swift/BASS (Wang et al. 2019a), and the green circles denote AGNs from SDSS (Huang et al. 2022). The top panel shows distributions of z for the two subsamples; the right panel shows their distributions of L 5100.
Paper: The σHβ -based Dimensionless Accretion Rate and Its Connection with the Corona for AGNs
Authors: Yu-Qin Chen, 玉琴 陈, Yan-Sheng Liu, 延盛 刘, Wei-Hao Bian, 维豪 卞
Figure caption: The distribution of FWHM/σ Hβ .
Paper: The σHβ -based Dimensionless Accretion Rate and Its Connection with the Corona for AGNs
Authors: Yu-Qin Chen, 玉琴 陈, Yan-Sheng Liu, 延盛 刘, Wei-Hao Bian, 维豪 卞
Figure caption: Distributions of the differences of M BH (left), ﹩\dot{M}﹩ (middle), and L Bol/L Edd (right) based on σ Hβ  and FWHMHβ .
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: Broadband SED model for the AGN continuum, which consists of a disk blackbody (dbb), a Comptonized disk component (comt), a power-law component (pow), and a reflection component (refl). NIR, UV, and X-ray spectra obtained with ground and space missions at different times are also shown. Both the model and data are corrected for the extinction (NIR and UV) and absorption (X-ray) effects. Observed data include emissions from warm emitter, BLR, dusty torus, and host galaxy, in addition to the intrinsic AGN SED. Data and model are rebinned for clarity.
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: Archival Swift XRT and UVOT observations of MR 2251-178 from 2014 January 9 to 2021 May 10. The top panel is the UVW2 flux. The two middle panels are the count rates in the hard (H: 1.5–10 keV) and soft (S: 0.3–1.5 keV) X-ray bands. The bottom panel shows the X-ray hardness ratio R = (H − S)/(H + S). The horizontal solid line in red is the historical average hardness ratio before late-2020. The vertical dashed line in purple marks the joint XMM-Newton + HST/COS + NuSTAR observation on 2020 December 16.
Paper: Multiwavelength Observations of the Obscuring Wind in the Radio-quiet Quasar MR 2251-178
Authors: Junjie Mao, G. A. Kriss, H. Landt, M. Mehdipour, J. S. Kaastra, J. M. Miller, D. Stern, L. C. Gallo, A. G. Gonzalez, J. J. Simon, S. G. Djorgovski, S. Anand, Mansi M. Kasliwal, V. Karambelkar
Figure caption: The broadband SED of MR 2251-178 with and without obscuration and absorption effects of ionized absorbers (Galactic absorption and extinction effects are excluded here). The upper panel shows the obscuration effect due to the X-ray obscurer (XO) in 2020. The pink curve in the lower panel includes the absorption effect by the X-ray warm absorber (WA) in 2002, while the purple curve includes both the obscuration effect by the obscurer and the absorption effect by the de-ionized warm absorber in 2020.