adsabs/AstroCLIMB huggingface dataset:
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Radio-to-IR SEDs of NGC 985, NGC 1365, NGC 4235, and MCG −6−30−15. In each panel, the data points in the IR band (≲500 μm), indicated by diamonds, are taken from Ichikawa et al. (2019). Filled and unfilled marks denote detected values and upper limits, respectively, and in the same way, the other data are plotted. Errors are shown for all data, except for the 22 GHz radio band as the error is unavailable from the original paper of Smith et al. (2020). The IR flux densities were measured with apertures of FWHMs ≳6″, much larger than those for the mm-wave flux densities (i.e., ≲0.″6). Best-fit AGN and host-galaxy templates are presented by solid blue and gray lines, respectively. Modified blackbody components, used to extrapolate the best-fit models to the lower-frequency regime, are presented by dashed lines with the original colors. A black-filled circle shows the peak flux density measured by the ALMA 12-m array. Its accompanying dotted–dashed black line represents a power law obtained by fitting the ALMA 12-m data in different spectral windows. The shaded area represents the uncertainty in the spectral slope. Additionally, the peak flux density measured by using an ALMA 7-m array data with a beam size of ∼4.″5–6.″5 is shown as a magenta circle. We note that only 22 objects have 7-m data. An orange pentagon indicates the flux density due to synchrotron plus free–free emission, expected by the SFR from the IR data obtained at resolutions coarser than 6″. Thus, this should be regarded as an upper contribution limit to the mm-wave flux density. The accompanying orange dotted–dashed line is a power law with an index of 0.1, which is expected for the free–free emission, likely dominant in the mm-wave band (see Equation (3)). Lower-frequency data at 3 and 22 GHz obtained by the Very Large Array (VLA) are shown as a red square and a green triangle, respectively. Particularly for the 22 GHz data, a power law with an index of 0.7 is shown by a green dotted–dashed line.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Scatter plot of the average beam size ﹩{({\theta }_{\mathrm{beam}}^{\min }\times {\theta }_{\mathrm{beam}}^{\mathrm{maj}})}^{1/2}﹩ vs. the object distance (D). Dotted, dotted–dashed, and dashed lines indicate required beam sizes to achieve the physical resolutions of 50 pc, 100 pc, and 250 pc, respectively, as a function of distance.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Left: histogram of the separation angle between the Chandra X-ray position and the identified mm-wave peak for 53 AGNs. The orange line shows a fitted Rayleigh distribution. Middle: same as the left panel, but for the WISE positions. The fitted Rayleigh distribution (orange line) has a smaller width than that fitted to the Chandra result, but several outliers appear. The objects named in blue have Chandra data, and such data are not found for those in black (Mrk 1310 and Mrk 520). Right: histogram on the separation angles for the AGN positions that we finally adopted in searching for mm-wave peaks. Chandra, WISE, and Gaia only for Mrk 1310 are adopted in that order for the AGN positions.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Histograms of essential parameters for our sample and the parent sample of Ricci et al. (2017b; from the left top to the right bottom: distance, absorbing hydrogen column density measured in the X-ray band, 14–150 keV luminosity, black hole mass, Eddington ratio, and bolometric luminosity). The histograms of D, M BH, λ Edd, and L bol are composed of all 98 AGNs, whose black hole masses were measured either by Koss et al. (2017) or by Koss et al. (2022c). Those of N H, and L 14−150 also include all 98 AGNs, and the values were taken from Ricci et al. (2017b). The bolometric luminosities, necessary to derive the Eddington ratios, were calculated based on a 2–10 keV-to-bolometric correction factor of Duras et al. (2020). The histograms for the parent sample are rescaled by a factor of 0.2 to be easily compared with those of our sample.
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption: Left: u’-band stacked CFHT image of the host galaxy of SN 2019jc. The SN location is marked by a 1.5 kpc diameter aperture. Right: a histogram comparing the estimated SFR density at the location of SN 2019jc (orange) with SFR densities at the locations of SESNe from Galbany et al. (2018; blue) and USSNe (green). The value we measure at the location of iPTF14gqr is an upper limit, marked by a dashed green line and left-pointing arrow. SN 2019jc lies at the very lower edge of the SESN distribution.
Paper: The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
Authors: C. Pellegrino, D. A. Howell, G. Terreran, I. Arcavi, K. A. Bostroem, P. J. Brown, J. Burke, Y. Dong, A. Gilkis, D. Hiramatsu, G. Hosseinzadeh, C. McCully, M. Modjaz, M. Newsome, E. Padilla Gonzalez, T. A. Pritchard, D. J. Sand, S. Valenti, M. Williamson
Figure caption: A spectrum of SN 2019hgp compared with the USSN model spectrum at maximum light from Moriya et al. (2017), the USSN SN 2005ek (Drout et al. 2013), the prototypical Type Ibn SN 2006jc, and the normal Type Ic SN 2007gr. Spectra of SN 2006jc, SN 2005ek, and SN 2007gr were obtained from WiseRep (Yaron & Gal-Yam 2012). Phases are denoted to the right of each spectrum. Possible spectral features are marked with dashed lines. SN 2019hgp shares several features with the USSNe at these phases.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Plot of 14–150 keV luminosity vs. redshift for our sample (blue) and the parent sample of Ricci et al. (2017b; gray). The area covered by ﹩\mathrm{log}[{L}_{14-150}/(\mathrm{erg}\,{{\rm{s}}}^{-1})]\gt 42﹩ and z < 0.01 is adopted to select AGNs to investigate the Malmquist bias (Section 5.2).
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Histogram of the rest frequencies at which our targets were observed by ALMA.
Paper: Hi-C 2.1 Observations of Reconnection Nanojets
Authors: Ritesh Patel, Vaibhav Pant
Figure caption: (a) Full-disk image of the Sun at 171 Å of AIA. Red box represents the Hi-C FOV that is shown in the (b). The locations of the identified nanojets are marked by “+” symbol in the Hi-C FOV in white.
Paper: Hi-C 2.1 Observations of Reconnection Nanojets
Authors: Ritesh Patel, Vaibhav Pant
Figure caption: Multiwavelength AIA observations of the two nanojets, N1 and N2, observed in Hi-C FOV. The upper and lower panels correspond to the two nanojets observed in AIA 304, 131, 171 and 193 Å, respectively, from left to right.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Coupling maps for each port with no vortex (top left), and a charge 1 (top middle) and charge 2 (top right) vortex. The maps span −3 λ/D to 3 λ/D in each direction. Bottom left: throughput line profiles with no vortex. The four nulled ports satisfying ﹩l\pm m^{\prime} =0﹩ are LP11ab and LP21ab. Bottom middle: throughput line profiles with a charge 1 vortex. The four nulled ports satisfying ﹩l\pm m^{\prime} =0﹩ are LP01, LP21ab, and LP02. Bottom right: throughput line profiles for each port with a charge 2 vortex. The four nulled ports satisfying ﹩l\pm m^{\prime} =0﹩ are LP01, LP11ab, and LP02. Although nulls in the LP21ab ports are not guaranteed by symmetry, in this case, their central throughputs are spuriously low, and including them in the data analysis may provide some additional gains.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Line profiles for summed throughput of nulled ports for PLNs with no vortex (left), a charge 1 vortex (middle), and a charge 2 vortex (right), using MSPLs with varying numbers of output ports. As the number of ports increases, each additional port brings decreasing returns in additional throughput. The current limit of what can be practically manufactured is six ports. Thus, we choose to use a six-port MSPL in our PLN design, which balances the total throughput of the nulled ports with what is practically manufacturable. Note that a higher V number of 8.48 was necessary to generate up to 19 LP modes. Here, we wish to compare the effect of port number independently of V number effects, so fix the V number at 8.48 for all port numbers. Thus, due to the difference in V number, the line profiles shown in this analysis have slightly different shapes from those in Figure 3.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Stellar coupling rate as a function of individual Zernike polynomial amplitude, with no vortex (top), a charge 1 vortex (middle), and a charge 2 vortex (bottom). For the nulled ports, solid lines indicate modes predicted to couple (those satisfying ﹩l\pm (m^{\prime} +m)=0﹩), while dashed lines indicate modes that are not predicted to couple (to first order, though higher-order coupling effects can be seen). Values of η  s  falling below 10−6 are likely numerical noise, and are not shown. Lines that fall entirely below 10−6 are light gray in the legend.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Left: stellar coupling rates as a function of tip-tilt jitter, random-uniformly distributed in position angle, with no vortex (left), a charge 1 vortex (middle), and a charge 2 vortex (right). The standard deviation of the per-frame tip-tilt amplitude is given by σ tt, with the position angle drawn uniformly between 0 and 2π.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: (a) Schematic of a focal-plane VFN with a single-mode fiber. The beam is focused onto a vortex mask, which imparts a different phase pattern on the star and planet PSFs. The beam is then collimated and refocused onto a single-mode fiber. The on-axis starlight is rejected while the planet light gets partially coupled. (b) Coupling efficiency, η, or throughput, of a planet as a function of its angular separation from the star.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Left: schematics of a six-port MSPL spatial-multiplexer fiber system. Each LP mode at the FMF face is mapped to one of the six single-mode ports of the SMF face, such that light with an LP mode shape at the FMF side will result in flux in the corresponding SMF core. The device is bidirectional, so light injected into one of the SMF ports will propagate into the LP mode corresponding to that port at the FMF face. Right: the field amplitudes of the first six LP modes, corresponding to the ideal modes of a six-port MSPL.
Paper: X-Rays in Cepheids: Identifying Low-mass Companions of Intermediate-mass Stars 
Authors: Nancy Remage Evans, Scott Engle, Ignazio Pillitteri, Edward Guinan, H. Moritz Günther, Scott Wolk, Hilding Neilson, Massimo Marengo, Lynn D. Matthews, Sofia Moschou, Jeremy J. Drake, Elaine M. Winston, Maxwell Moe, Pierre Kervella, Louise Breuval
Figure caption: X-ray observations of Cepheids. Upper limits from nondetections in Table 2 are filled red downward-pointing arrows. Detections of Cepheids in Table 3 are as follows: δ Cep (connected open squares), Polaris (connected crosses), and β Dor (connected triangles). The solid portion of the Polaris data line shows the phase range of the new observation in Table 1. For η Aql and SU Cas upper limits are indicated and the lines show the phase range covered. The mean log L X for F, G, and K main-sequence stars is shown by the dashed line at log L X = 29.6. Circles in the upper left corner (labeled) are systems where the low-mass companion dominates the X-rays (Table 4). Luminosity is in erg s−1.
Paper: X-Rays in Cepheids: Identifying Low-mass Companions of Intermediate-mass Stars 
Authors: Nancy Remage Evans, Scott Engle, Ignazio Pillitteri, Edward Guinan, H. Moritz Günther, Scott Wolk, Hilding Neilson, Massimo Marengo, Lynn D. Matthews, Sofia Moschou, Jeremy J. Drake, Elaine M. Winston, Maxwell Moe, Pierre Kervella, Louise Breuval
Figure caption: Our X-ray survey demonstrates that ﹩{28}_{-9}^{+13} \% ﹩ of Cepheids have unresolved late F/G/K companions across q = 0.10–0.28 (red). Meanwhile, an earlier UV survey (Evans 1992) found that 21% ± 5% of Cepheids have unresolved B/early A companions across q = 0.37–1.0 (magenta). The measured mass ratio distribution is inconsistent with both a uniform distribution (dotted) and random pairings of the IMF (dashed). We fit a power-law distribution with an intermediate slope of γ = −1.2 ± 0.4 across q = 0.1–1.0 (blue). The data are also consistent with the segmented power-law model adopted in Moe & Di Stefano (2017; green). In total, we find that 57% ± 12% of Cepheids have companions across q = 0.1–1.0 and a = 1–1000 au.
Paper: X-Rays in Cepheids: Identifying Low-mass Companions of Intermediate-mass Stars 
Authors: Nancy Remage Evans, Scott Engle, Ignazio Pillitteri, Edward Guinan, H. Moritz Günther, Scott Wolk, Hilding Neilson, Massimo Marengo, Lynn D. Matthews, Sofia Moschou, Jeremy J. Drake, Elaine M. Winston, Maxwell Moe, Pierre Kervella, Louise Breuval
Figure caption: Companion detection sensitivity for Cepheids from Gaia EDR3. Sensitivity for companion mass is shown as a function of orbital radius and orbital period. Green line: limit from proper-motion anomaly; blue line: limit for common proper motions; yellow dashed line: stellar mass limit; pink dashed line: brown dwarf limit; orbital period in years is shown by the pink lines on the x-axis. Cepheid parameters are 5.0 M ⊙ and 700 pc, typical parameters in this study. The green region above the stellar limit indicates that stellar companions at the low-mass stellar limit will be detected for orbital periods between about 3 and 100 yr.
Paper: X-Rays in Cepheids: Identifying Low-mass Companions of Intermediate-mass Stars 
Authors: Nancy Remage Evans, Scott Engle, Ignazio Pillitteri, Edward Guinan, H. Moritz Günther, Scott Wolk, Hilding Neilson, Massimo Marengo, Lynn D. Matthews, Sofia Moschou, Jeremy J. Drake, Elaine M. Winston, Maxwell Moe, Pierre Kervella, Louise Breuval
Figure caption: (a) The V659 Cen system. The diagram of the components indicates the Cepheid and the spectral types of the close and distant binary. Star Ab is a low-mass star (FGK) that produces the X-rays. The separations of the systems in au are indicated at the bottom. (The separation in the Aa–Ab binary is only an estimate.) (b) The W Sgr system, with the same notation as in panel (a).
Paper: X-Rays in Cepheids: Identifying Low-mass Companions of Intermediate-mass Stars 
Authors: Nancy Remage Evans, Scott Engle, Ignazio Pillitteri, Edward Guinan, H. Moritz Günther, Scott Wolk, Hilding Neilson, Massimo Marengo, Lynn D. Matthews, Sofia Moschou, Jeremy J. Drake, Elaine M. Winston, Maxwell Moe, Pierre Kervella, Louise Breuval
Figure caption: Multiwavelength observations of l Car as a function of pulsation phase. Panels top to bottom show emission lines from HST COS spectra, emission lines from IUE spectra, X-ray observations, V photometry, and radial velocities as discussed in the text.
Paper: X-Rays in Cepheids: Identifying Low-mass Companions of Intermediate-mass Stars 
Authors: Nancy Remage Evans, Scott Engle, Ignazio Pillitteri, Edward Guinan, H. Moritz Günther, Scott Wolk, Hilding Neilson, Massimo Marengo, Lynn D. Matthews, Sofia Moschou, Jeremy J. Drake, Elaine M. Winston, Maxwell Moe, Pierre Kervella, Louise Breuval
Figure caption: Multiwavelength observations of Polaris as a function of pulsation phase. Panels top to bottom show N V emission lines and Si IV emission lines from HST COS spectra, X-ray observations, V photometry, and radial velocities as discussed in the text. The error bars on the X-ray phases indicate the time period covered by the observations. The Chandra observation in Table 1 has been broken into two parts.
Paper: Polarized Image of a Rotating Black Hole in Scalar–Tensor–Vector–Gravity Theory
Authors: Xin Qin, Songbai Chen, Zelin Zhang, Jiliang Jing
Figure caption: Effects of the MOG parameter α on the polarized vector and EVPA in the Kerr–MOG black hole spacetime (3) for the different observer inclination angle θ  o . Here r  s  = 6, a = −0.3, β  ν  = 0.3, χ = −90°, B  r  = 0.87, B  ϕ  = 0.5, and B  θ  = 0.
Paper: Polarized Image of a Rotating Black Hole in Scalar–Tensor–Vector–Gravity Theory
Authors: Xin Qin, Songbai Chen, Zelin Zhang, Jiliang Jing
Figure caption: Effects of the MOG parameter α on the polarized vector and EVPA in the Kerr–MOG black hole spacetime (3) for the magnetic field owned only the radial component B  r . Here we set ﹩{ \mathcal M }\,=\,1﹩, r  s  = 6, θ  o  = 20°, β  ν  = 0.3, and χ = −90°.
Paper: Polarized Image of a Rotating Black Hole in Scalar–Tensor–Vector–Gravity Theory
Authors: Xin Qin, Songbai Chen, Zelin Zhang, Jiliang Jing
Figure caption: Effects of the MOG parameter α on the polarized vector and EVPA in the Kerr–MOG black hole spacetime (3) for the equatorial magnetic field owned only the angular component B  ϕ . Here we set ﹩{ \mathcal M }\,=\,1﹩, r  s  = 6, θ  o  = 20°, β  ν  = 0.3, and χ = −90°.
Paper: Polarized Image of a Rotating Black Hole in Scalar–Tensor–Vector–Gravity Theory
Authors: Xin Qin, Songbai Chen, Zelin Zhang, Jiliang Jing
Figure caption: Effects of the MOG parameter α on the polarized vector and EVPA in the Kerr–MOG black hole spacetime (3) for the different fluid direction angle χ. Here r  s  = 6, a = −0.3, θ  o  = 20°, β  ν  = 0.3, B  r  = 0.87, B  ϕ  = 0.5, and B  θ  = 0.
Paper: Polarized Image of a Rotating Black Hole in Scalar–Tensor–Vector–Gravity Theory
Authors: Xin Qin, Songbai Chen, Zelin Zhang, Jiliang Jing
Figure caption: Effects of the MOG parameter α on the polarized vector and EVPA in the Kerr–MOG black hole spacetime (3) for the equatorial magnetic field. Here r  s  = 6, a = −0.3, θ  o  = 20°, β  ν  = 0.3, and χ = −90°.
Paper: A Mildly Relativistic Outflow Launched Two Years after Disruption in Tidal Disruption Event AT2018hyz
Authors: Y. Cendes, E. Berger, K. D. Alexander, S. Gomez, A. Hajela, R. Chornock, T. Laskar, R. Margutti, B. Metzger, M. F. Bietenholz, D. Brethauer, M. H. Wieringa
Figure caption: Luminosity light curve over time of AT2018hyz in several frequency bands, including early upper limits (triangles) and the late-time detections starting at about 970 days (circles). While the source is rising in all frequencies during the first radio detections, we find the source has begun to fade in the L band (1.4 GHz, yellow) and the S band (3.0 GHz, green) after ∼1250 days. In contrast, at higher frequencies such as the C band (5.5 GHz, light blue), X band (9 GHz, dark blue), Ka band (14 GHz, purple), K band (19–20 GHz, pink), and in the millimeter band (97.5 GHz, brown; and 240 GHz, black) the source is still rising as roughly F  ν  ∝ t 5 through 1300 days. In the UHF band (0.88 GHz, red) we see the source has risen in luminosity ∼2.25×  from 1000 to 1280 days but do not have enough sampling to establish whether it is decreasing.