adsabs/AstroCLIMB huggingface dataset:
Paper: A Radio-selected Population of Dark, Long Gamma-Ray Bursts: Comparison to the Long Gamma-Ray Burst Population and Implications for Host Dust Distributions
Authors: Genevieve Schroeder, Tanmoy Laskar, Wen-fai Fong, Anya E. Nugent, Edo Berger, Ryan Chornock, Kate D. Alexander, Jennifer Andrews, R. Shane Bussmann, Alberto J. Castro-Tirado, Armaan V. Goyal, Charles D. Kilpatrick, Maura Lally, Adam A. Miller, Peter Milne, Kerry Paterson, Alicia Rouco Escorial, Michael C. Stroh, Giacomo Terreran, Bevin Ashley Zauderer
Figure caption: Swift/BAT fluence (f  γ ) in the 15–150 keV band vs. duration (T 90) of 976 typical GRBs (blue points) and 103 dark GRBs (red squares), as derived by Lien et al. (2016). Dark GRB classification is based on the either explicit classification, or satisfying β OX > −0.5 (Cenko et al. 2009; Krühler et al. 2011, 2012; Melandri et al. 2012; Rossi et al. 2012; Perley et al. 2013; Hunt et al. 2014; Schady et al. 2014; Jeong et al. 2014; Littlejohns et al. 2015; Perley et al. 2016a; Chrimes et al. 2019; this work). The dashed horizontal line represents the theoretical minimum ﹩{f}_{\gamma ,\min }\,\approx \,2.5\times {10}^{-7}\,\mathrm{erg}/{\mathrm{cm}}^{2}﹩, below which the X-ray (and therefore optical) afterglow is typically too faint to be classified as dark with ground-based rapid optical follow-up that reaches limits of R > 24 mag. A simple two-sample Kolmogorov–Smirnov (K-S) test from the scipy.stats package, which tests the null hypothesis that dark GRBs are drawn from the same population as the typical GRB population, finds p = 0.0001 for the f  γ  distribution and p = 0.0503 for the T 90 distribution, where a value of p < 0.05 rejects the null hypothesis.
Paper: A Radio-selected Population of Dark, Long Gamma-Ray Bursts: Comparison to the Long Gamma-Ray Burst Population and Implications for Host Dust Distributions
Authors: Genevieve Schroeder, Tanmoy Laskar, Wen-fai Fong, Anya E. Nugent, Edo Berger, Ryan Chornock, Kate D. Alexander, Jennifer Andrews, R. Shane Bussmann, Alberto J. Castro-Tirado, Armaan V. Goyal, Charles D. Kilpatrick, Maura Lally, Adam A. Miller, Peter Milne, Kerry Paterson, Alicia Rouco Escorial, Michael C. Stroh, Giacomo Terreran, Bevin Ashley Zauderer
Figure caption: Top: distribution of inferred stellar masses ﹩({\mathrm{log}}_{10}({M}_{* }/{M}_{\odot }))﹩ of the hosts of 82 typical GRBs (blue) and the hosts of 68 dark GRBs (red), gathered from the literature (Savaglio et al. 2009; Leibler & Berger 2010; Perley et al. 2013; Hunt et al. 2014; Piranomonte et al. 2015; Perley et al. 2016b; Japelj et al. 2016; Palmerio et al. 2019, this work). Available upper limits are denoted by the dashed, unfilled distribution with leftward arrow. The hosts of the dark GRB population are generally more massive than the typical GRB population (median ﹩{\mathrm{log}}_{10}({M}_{* }/{M}_{\odot })\approx 9.9﹩ for the hosts of dark GRB population, vs. median ﹩{\mathrm{log}}_{10}({M}_{* }/{M}_{\odot })\approx 9.2﹩ for the typical GRB population). Bottom: distribution of extinction, A  V,Host, of 92 typical GRB hosts (blue) and 60 dark GRB hosts (red), gathered from the literature (Savaglio et al. 2009; Perley et al. 2013; Hunt et al. 2014; Krühler et al. 2015; Piranomonte et al. 2015; Japelj et al. 2016; this work), where upper limits are denoted by the dashed, unfilled distribution with leftward arrow. The hosts of the dark GRB population are generally more dusty than the typical GRB population (median A  V,Host ≈ 1.1 mag for the hosts of dark GRB population, vs. median A  V,Host ≈ 0.5 mag for the typical GRB population).
Paper: A Radio-selected Population of Dark, Long Gamma-Ray Bursts: Comparison to the Long Gamma-Ray Burst Population and Implications for Host Dust Distributions
Authors: Genevieve Schroeder, Tanmoy Laskar, Wen-fai Fong, Anya E. Nugent, Edo Berger, Ryan Chornock, Kate D. Alexander, Jennifer Andrews, R. Shane Bussmann, Alberto J. Castro-Tirado, Armaan V. Goyal, Charles D. Kilpatrick, Maura Lally, Adam A. Miller, Peter Milne, Kerry Paterson, Alicia Rouco Escorial, Michael C. Stroh, Giacomo Terreran, Bevin Ashley Zauderer
Figure caption: Radio SFR (SFRRadio) vs. SED-derived SFR (SFRSED) for typical GRB host galaxies (blue) and dark GRB host galaxies (red). Triangles correspond to radio upper limits. SFRRadio is derived from radio observations in the literature (Perley & Perley 2013; Stanway et al. 2014; Perley et al. 2015; Greiner et al. 2016; Perley et al. 2017; Gatkine et al. 2020; Eftekhari et al. 2021) using the SFRRadio relation in Greiner et al. (2016) and assuming a spectral index of −0.75. SFRSED is taken from the literature (Perley et al. 2013, 2015) and supplemented with UV-derived SFR or SFR tracers such as H  α  (Hunt et al. 2014; Krühler et al. 2015). Our sample of six dark GRBs is shown as the filled-in red triangles, with SFRRadio from the most constraining radio afterglow upper limits and SFRSED from our Prospector host galaxy modeling. Also shown are a sample of star-forming galaxies for comparable redshifts z ≈ 0.03–3.4 from the VLA-COSMOS source catalog (gray; Smolčić et al. 2017). The dashed and dotted line indicate SFRRadio = SFRSED and SFRRadio = 10 × SFRSED, respectively.
Paper: A Radio-selected Population of Dark, Long Gamma-Ray Bursts: Comparison to the Long Gamma-Ray Burst Population and Implications for Host Dust Distributions
Authors: Genevieve Schroeder, Tanmoy Laskar, Wen-fai Fong, Anya E. Nugent, Edo Berger, Ryan Chornock, Kate D. Alexander, Jennifer Andrews, R. Shane Bussmann, Alberto J. Castro-Tirado, Armaan V. Goyal, Charles D. Kilpatrick, Maura Lally, Adam A. Miller, Peter Milne, Kerry Paterson, Alicia Rouco Escorial, Michael C. Stroh, Giacomo Terreran, Bevin Ashley Zauderer
Figure caption: Left: X-ray, optical, millimeter, and radio afterglow light curves of GRB 130131A, together with the best-fit forward shock model in an ISM environment (lines). Squares represent data newly reported here, circles represent Swift/XRT data, and triangles represent 3σ upper limits. Open symbols indicate data that are not included in the fit, and shaded regions represent variability due to scintillation. The inset shows the model J- and R-band light curves (solid lines) as well as the nonextinguished models (dashed lines), indicating A  V,GRB ≈ 2.4 mag to explain the detections. Right: radio and millimeter spectral energy distributions (SEDs) of the afterglow of GRB 130131A from δ t ≈ 0.7–13.9 days, together with the best-fit forward shock model (lines).
Paper: A Radio-selected Population of Dark, Long Gamma-Ray Bursts: Comparison to the Long Gamma-Ray Burst Population and Implications for Host Dust Distributions
Authors: Genevieve Schroeder, Tanmoy Laskar, Wen-fai Fong, Anya E. Nugent, Edo Berger, Ryan Chornock, Kate D. Alexander, Jennifer Andrews, R. Shane Bussmann, Alberto J. Castro-Tirado, Armaan V. Goyal, Charles D. Kilpatrick, Maura Lally, Adam A. Miller, Peter Milne, Kerry Paterson, Alicia Rouco Escorial, Michael C. Stroh, Giacomo Terreran, Bevin Ashley Zauderer
Figure caption: Left: X-ray, optical, millimeter, and radio afterglow light curves of GRB 140713A, together with the best-fit forward shock model in an ISM environment (lines). Squares represent data newly reported here, circles represent literature data (Higgins et al. 2019), and triangles represent 3σ upper limits. Open symbols indicate data that are not included in the fit, and shaded regions represent variability due to scintillation. The inset shows the model r-, i-, and z-band light curves (solid lines) as well as the nonextinguished models (dashed lines), indicating A  V,GRB ≳ 3.1 mag to explain the upper limits. Right: radio and millimeter SEDs of the afterglow of GRB 140713A from δ t ≈ 3.0–31.5 days, together with the best-fit forward shock model (lines).
Paper: A Radio-selected Population of Dark, Long Gamma-Ray Bursts: Comparison to the Long Gamma-Ray Burst Population and Implications for Host Dust Distributions
Authors: Genevieve Schroeder, Tanmoy Laskar, Wen-fai Fong, Anya E. Nugent, Edo Berger, Ryan Chornock, Kate D. Alexander, Jennifer Andrews, R. Shane Bussmann, Alberto J. Castro-Tirado, Armaan V. Goyal, Charles D. Kilpatrick, Maura Lally, Adam A. Miller, Peter Milne, Kerry Paterson, Alicia Rouco Escorial, Michael C. Stroh, Giacomo Terreran, Bevin Ashley Zauderer
Figure caption: X-ray, optical, and radio afterglow light curves of GRB 110709B, together with the best-fit forward shock model in an wind environment (lines). Circles represent literature data (Zauderer et al. 2013c), and triangles represent 3σ upper limits. Open symbols indicate data that are not included in the fit, and shaded regions represent variability due to scintillation. The inset shows the model K  s -band and H-band light curves (solid lines) as well as the nonextinguished models (dashed lines), indicating A  V,GRB ≳ 5.0 mag to explain the upper limits.
Paper: X-Ray and Radio Observations of Central Black Holes in Nearby Low-mass Early-type Galaxies: Preliminary Evidence for Low Eddington Fractions
Authors: Ryan Urquhart, Lauren I. McDermott, Jay Strader, Anil C. Seth, Laura Chomiuk, Nadine Neumayer, Dieu D. Nguyen, Evangelia Tremou
Figure caption: Nearest low-mass early-type galaxies have low accretion rates. The solid lines and regions show the cumulative distribution function of L bol/L Edd distributions of bright, massive galaxies based on X-ray measurements from Ho (2009) assuming L bol = 15.8L  X . The black lines shows the full galaxy sample (175 galaxies), while the red lines show just the early-type galaxies (93 galaxies). The shaded regions in both samples show the impact of upper limits on the cumulative distribution functions. The three dashed lines, from left to right, show the L bol/L Edd measurements for M32, NGC 5102, and NGC 404, while the dotted line shows the upper limit on L bol/L Edd for NGC 205, assuming a black hole mass of 6800 M ⊙.
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: (a) Spectra of Ref1 taken in 2000 (black), 2003 (red), 2007 (magenta), 2009 (green), and 2015 (blue). The best-fit models are shown as the stepped lines. The dashed line and dotted line are the NEI component and the nonthermal component, respectively. (b)–(f) Spectra of Knot1 taken in 2000, 2003, 2007, 2009, and 2015. The solid lines are the soft components. The other lines represent the same components as panel (a).
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: Soft (a), middle (b), and hard (c) band X-ray images around Knot1 taken in 2000, 2003, 2007, 2009, and 2015. All of the images are exposure corrected. In all of the panels, the unit for the color scale is photons s−1 cm−2. Contours represent the flux of the soft-band X-rays. The green ellipses are the Knot1, Ref1, and Ref2 regions used for spectral extraction, respectively.
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: Time variations of kT  e  (left), n  e  t (middle), and EMs (right) of the best-fit soft component of Knot1. The black and gray plots represent the best-fit parameters when n  e  t is fixed and free, respectively.
Paper: X-Ray and Radio Observations of Central Black Holes in Nearby Low-mass Early-type Galaxies: Preliminary Evidence for Low Eddington Fractions
Authors: Ryan Urquhart, Lauren I. McDermott, Jay Strader, Anil C. Seth, Laura Chomiuk, Nadine Neumayer, Dieu D. Nguyen, Evangelia Tremou
Figure caption: Left: Chandra image of NGC 205 smoothed using a Gaussian tophat 2 pixels wide for visualization purposes. The red cross marks the optical nucleus. Middle: as in left, but for the HST/WFC3 F555W image. Right: as in left, but for the 6 GHz VLA image. The beam size is indicated by the white ellipse in the lower left corner. Contours are set at ﹩2\sqrt{{2}^{n}}\times \sigma ﹩, where σ is the local rms (σ = 1.1 μ Jy beam−1) and n = 1, 2, 3, 4.... The source is not detected in either the radio or X-ray image.
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: (a) Difference image of Tycho between 2003 and 2015 in the 0.5–1.5 keV band, where Ne-Kα and Fe-L lines are dominated. The unit for the color scale is photons s−1 cm−2. Knot1 is located in the box region. (b) Enlarged image of the box region indicated in panel (a). The circle is the region where the flux changes significantly.
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: Comparison of the spectra of Knot1 (black) and the best-fit model of Ref1 for the effective area of Knot1 (red) in 2000, 2003, 2007, 2009, and 2015. The model is composed of an NEI component and a power-law component as explained in the text. Lower panels in each box show the ratio of the data of Knot1 to the model of Ref1.
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: The spectra and the best-fit model of Ref2 taken in 2000 (black), 2003 (red), 2007 (magenta), 2009 (green), and 2015 (blue). The lines show the model whose parameters, except for EM, are fixed to those of Ref1. The components represent the same ones as Figure 4.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Projected phase-space diagrams of our sample (star symbols) and the GASP jellyfish galaxies (circles). We normalize clustercentric distance (R cl) and absolute relative velocity (∣v los∣) with cluster virial radius (R 200) and velocity dispersion (σ  v,cl), respectively. All of the data are color-coded by total SFR (left) and tail SFR (right). The color bars on the top denote the logarithmic scale of each SFR. Gray dashed lines represent the boundaries of the five regions that were roughly defined by infall stages of cluster galaxies (Rhee et al. 2017; Mun et al. 2021): Region A (first infall), B (recent infall), C (intermediate infall), D (ancient infall), and E (field). We divide the whole sample into three categories by stellar mass: low-mass (M * < 5 × 109 M ⊙;  upper), intermediate-mass (5 × 109 M ⊙ < M * < 5 × 1010 M ⊙;  middle), and high-mass (M * > 5 × 1010 M ⊙;  lower) galaxies.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Upper left: HST color image of MACSJ0916-JFG1 overlaid with the Hα flux contour (magenta solid lines) derived from the GMOS/IFU data. We mark the orientation, distance scale, and redshift of this galaxy. Upper right: the SFR density (Σ SFR ) map estimated from the Hα luminosity. The red dashed circle represents the boundary of the disk and tail of this galaxy. Gray contours denote the spatial distribution of Hα flux. The right color bar shows the scale and range of the values. Lower left: the radial velocity map derived from the peak wavelength of Hα emission line. We display the relative velocity of each bin with respect to the central Voronoi bin with the highest Hα flux. Lower right: the gas velocity dispersion map derived from the width of Hα emission line.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Same as Figure 12, but we divide the sample into three categories by cluster velocity dispersion: low-mass (σ  v,cl < 600 km s−1;  upper), intermediate-mass (600 km s−1 < σ  v,cl < 900 km s−1;  middle), and high-mass (σ  v,cl > 900 km s−1;  lower) clusters.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Left panels: BPT diagrams of the Voronoi bins with S/N > 3 in MACSJ1752-JFG2 (upper: a non-AGN host galaxy) and MACSJ1258-JFG1 (lower: an AGN host galaxy). The colors of the circular symbols represent the BPT classifications: star-forming (blue), composite (orange), and AGN+LINER regions (green). We color-code each symbol with the value of log ([O III] λ5007/Hβ). Right panels: spatial maps of the regions classified in the BPT diagrams. Here we exclude the Voronoi bins with S/Ns less than 3. The red dashed ellipse represents the boundary of the disk and tail of this galaxy. The orientation and distance scale are marked in the figure.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: A BPT diagram of the integrated spectra of the five jellyfish galaxies. Each galaxy is marked with the same order as in Figure 2: (a) MACSJ0916-JFG1, (b) MACSJ1752-JFG2, (c) A2744-F0083, (d) MACSJ1258-JFG1, and (e) MACSJ1720-JFG1. We plot a solid line from Kauffmann et al. (2003), a dotted line from Kewley et al. (2001), and a dashed line from Sharp & Bland-Hawthorn (2010) to divide star-forming, composite, AGN, and LINER regions in this diagram.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Same as Figure 7 but for MACSJ1720-JFG1.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Same as Figure 7 but for A2744-F0083.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Same as Figure 7 but for MACSJ1752-JFG2.
Paper: A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Jeong Hwan Lee, Myung Gyoon Lee, Jae Yeon Mun, Brian S. Cho, Jisu Kang
Figure caption: Same as Figure 7 but for MACSJ1258-JFG1.
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: The relation between the black hole mass and the deprojected distance of the jet collimation break from the central engine. The red star shows our results from the 3C 273 jet, and the cyan circles show results from other sources reported in the literature. The red horizontal bar indicates the region of a persistent feature seen near the break distance with a complex bending double-ridge-like morphology potentially associated with the transition in the jet shape (see Figure 9 and Section 6.1). To compare with the location of the SGI, we show the SGI locations of the classical bulges and elliptical galaxies in gray squares taken from Kormendy & Ho (2013). The black solid line and gray shaded area are the best-fit model and the 1σ error range of the relation between the black hole mass and SGI location, transformed from the M BH–σ  d  relation in Kormendy & Ho (2013). The dotted lines show the actual distances in parsecs. The results of other sources are obtained from the following references; M87: Asada & Nakamura (2012), NGC 6251: Tseng et al. (2016), NGC 4261: Nakahara et al. (2018), Cygnus A: Nakahara et al. (2019), NGC 1052: Nakahara et al. (2020), NGC 315: Park et al. (2021), 4C 38.41: Algaba et al. (2019), 3C 264: Boccardi et al. (2019), 1H 0323+342: Hada et al. (2018), and other sources: Kovalev et al. (2020). Note that we show two cases of different black hole masses for 1H 0323+342 (see Section 6.2).
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: The radius and PA of the 3C 273 jet as a function of the deprojected distance from the central black hole. The deprojected distance from the central black hole is derived using the best-fit core shift model at a viewing angle of i = 9° (see Section 1) for the black hole mass of M BH = 2.6 × 108  M ⊙ (Gravity Collaboration et al. 2018). Upper panel: the jet radius profile. The colored circles and associated error bars indicate the mean values and standard deviations of the measurements, respectively. Different colors show measurements from different observations, as shown in the legend. The solid and dashed lines show single power-law fits (r ∝ z  a ) to the inner side, semiparabolic (a = 0.66), and to the outer side, conical/hyperbolic (a = 1.28), respectively. The surrounding shaded areas represent the uncertainty of the single power-law fits (1σ, 2σ, 3σ). The green line represents the best-fit broken power-law function, giving the best-fit distance of the jet shape break of z  b  = 1.1 × 107 R s shown on the vertical dotted line. Lower panel: the jet PA profile. The color convention is the same as in the upper panel. The horizontal dashed line shows PA = −138°, which is broadly consistent with the axis of the large-scale jet (e.g., Davis et al. 1985; Conway et al. 1993). The gray shade across both panels shows the region excluded from the fitting analysis because of a large bending seen in the jet (see the details in Section 5.5).
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: One of the top-set images from HSA 15 GHz observation (gray contours) overlaid with the streamline of the 3C 273 jet (filled and open circles). The regions excluded from our fitting are indicated by gray filled circles, showing a stable complex and bending double-ridge-like morphology not seen in the rest of the global jet (see Section 6.1). A black dashed line indicates the global position angle of the jet estimated from the large-scale jet image (e.g., Davis et al. 1985).