adsabs/AstroCLIMB huggingface dataset:
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: Estimate of the slope of the lag–wavelength relation across the wavelength range of ZTF filters for BLR emission, including diffuse continuum emission and an Hα line with a FWHM of 6000 kms−1. The Hα lag is assumed to be 10 days. The lag spectrum of diffuse BLR emission is from Korista & Goad (2019) with hydrogen column density ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})=23﹩ and hydrogen gas density ﹩\mathrm{log}({n}_{{\rm{H}}}/{\mathrm{cm}}^{-3})﹩ integrated from 8 to 12 dex. A typical redshift of z ∼ 0.1 is assumed. The orange dashed line indicates the ZTF i-band transmission function. Three lag values at the effective wavelengths of ZTF filters are fitted with Equation (1).
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: Properties of the initial sample. Panels (a) and (b) show the redshift and mean magnitude distributions, respectively. Different colors represent different bands as shown in the label. Panels (c)–(e) display the distributions of number of epochs, cadence, and square root of excess variance of the light curves. Panel (f) shows the distribution of the radio flux density.
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: Observed-frame lag comparison between ICCF and JAVELIN methods. Both g − r and g − i lags, their uncertainties, and sample size are shown in each panel. The 1:1 ratio is indicated by the black dashed line.
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: ICCF rest-frame lag measurements for the parent and core samples. The gray and red dots are inter-band lags with 1σ uncertainties in the parent and core samples, respectively. The gray and red lines correspond to the best linear fits through zero. The 1:1 ratio is marked with the black dotted line.
Paper: Active Galactic Nuclei Continuum Reverberation Mapping Based on Zwicky Transient Facility Light Curves
Authors: Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Shu Wang
Figure caption: Distributions of β in the parent and core samples. The SSD prediction of β = 4/3 is indicated by the black dashed line.
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: Deep optical or NIR observations of the fields of GRBs 130131A, 130420B, 130609A, 131229A, 140713A, and 160509A. In each panel, the blue solid-line circle indicates the XRT afterglow location (90% confidence). When available, the red circle indicates the radio afterglow location (1σ), the green circle denotes the optical or NIR position (1σ), and the dashed blue circle indicates the CXO position. Images have been smoothed with a 3-pixel Gaussian, and the orientation is north up and east to the left. An angular scale is provided in all images, in addition to a physical scale when the redshift is known. For GRBs 130420B and 130609A, we do not identify host galaxies.
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 111215A, together with the best-fit forward shock model in a wind environment (lines). Circles represent literature data (Zauderer et al. 2013c; van der Horst et al. 2015), 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 ﹩z^{\prime} ﹩-, J-, and Ks -band light curves (solid lines) as well as the nonextinguished models (dashed lines), indicating A  V,GRB ≳ 10.6 mag to explain the upper limits. Right: radio and millimeter SEDs of the afterglow of GRB 111215A from δ t ≈ 1.5–88.23 days, together with the best-fit forward shock model (lines). Overall the model provides a good match to the broadband temporal and spectral evolution of the afterglow.
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, NIR, millimeter, and radio afterglow light curves of GRB 130131A, together with the best-fit forward shock model in a wind 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 ≈ 2.2 mag to explain the detections. Right: radio and millimeter SEDs of the afterglow of GRB 130131A from δ t ≈ 0.7−13.9 days, together with the best-fit forward shock model (lines). Overall, the model provides a good match to the broadband temporal and spectral evolution of the afterglow.
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: radio to X-ray SED of GRB 131229A at 0.91 days, with observations (purple) and estimated ﹩{F}_{{\nu }_{{\rm{c}},\min }}﹩ at ﹩{\nu }_{{\rm{c}},\max }﹩ (green). The black solid line indicates the broken power-law fit between the 21.8 GHz upper limit and ﹩{F}_{{\nu }_{{\rm{c}}}}﹩, where the break indicates ν m ≈ 1013 Hz. The dashed line indicates the single power-law fit from the radio to X-ray frequencies. Right: optical to X-ray SED of GRB 131229A at 0.0368 days, with optical/NIR upper limits (purple) and estimated ﹩{F}_{{\nu }_{{\rm{c}},\min }}﹩ at ﹩{\nu }_{{\rm{c}},\max }﹩ (green). The dashed gray line represents the extrapolation from ﹩{F}_{{\nu }_{{\rm{c}},\max }}﹩ assuming ν m < NIR/optical < ν c with no extinction (A  V,GRB = 0 mag). The black solid line represents the extinction curve with the minimum extinction required to be consistent with the upper limits (A  V,GRB ≳ 9.6 mag).
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 a wind 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 ≳ 3.5 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). Overall, the model provides a good match to the broadband temporal and spectral evolution of the afterglow.
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: The observed host photometry (circles) of the dark GRBs modeled in this paper (GRBs 110709B, 111215A, 130131A, 131229A, and 160509A), as well as the Prospector model photometry (squares) and best-fit model spectrum (lines). For GRB 160509A, a second Prospector model is plotted that does not include the Hubble Space Telescope (HST)/WFC3 photometry of the host (dashed line; see Section 4 for details). The GRB SEDs are arbitrarily scaled in flux for clarity.
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: The grizJK and Spitzer photometry (purple circles) of GRB140713A compared to the Prospector-produced model spectrum (purple line) and photometry (green squares) at z = 0.935. The model is consistent with the observed photometry across the wide wavelength range. The inset shows a zoomed-in image of the observed LRIS spectrum (purple line), as well as the error spectrum (gray line), compared to the model spectrum.
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 ISM environment (lines). Circles represent detections, and triangles represent 3σ upper limits (Zauderer et al. 2013c). 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), with A  V,GRB ≳ 3.9 mag necessary to be consistent with the upper limits.
Paper: The Volumetric Star Formation Law in the Almost Edge-on Galaxy NGC 4302 Revealed by the Atacama Large Millimeter/submillimeter Array
Authors: Kijeong Yim, Tony Wong, Richard J. Rand
Figure caption: Position–velocity diagrams integrated vertically for CO (top) and H I (middle). CO contours are 1.0 × 1.8 n  K arcseconds, with n = 0, 1, 2, 3, 4. H I contour levels are 175.0 × 1.5 n  K arcseconds, with n = 0, 1, 2, 3, 4. The lowest contour level is 5σ. The horizontal dotted lines indicate the heliocentric systemic velocity of 1140 km s−1. Bottom: rotation curves of CO (red squares) and H I (blue circles) obtained from p–v diagrams along the midplane. The rotation velocities are overlaid on the p–v diagrams as red filled circles. The uncertainties from the correction term in Equation (1) are shown in the upper left and right corners.
Paper: The Volumetric Star Formation Law in the Almost Edge-on Galaxy NGC 4302 Revealed by the Atacama Large Millimeter/submillimeter Array
Authors: Kijeong Yim, Tony Wong, Richard J. Rand
Figure caption: CO and H I integrated intensity maps. The northern disk is placed in negative x. Contour levels are 10.0 × 2.5 n  K km s−1, with n = 0, 1, 2, 3, 4 for CO and 750.0 × 1.6 n  K km s−1, with n = 0, 1, 2, 3 for H I. The lowest contour levels are ∼10σ for CO and ∼5σ for H I. The synthesized beam is shown in the lower right corner of each panel. The Spitzer 24 μm contour levels are 0.2 × 3.4 n  MJy sr−1, with n = 0, 1, 2, and 3 and the Hα contour levels are 0.0003 × 2.5 n  MJy sr−1, with n = 0, 1, and 2. The lowest contours are ∼10σ for 24 μm and ∼3σ for Hα. The point-spread function FWHM is shown in the lower right corner of each panel: 5.″9 for 24 μm  and 1.″5 for Hα.
Paper: The Volumetric Star Formation Law in the Almost Edge-on Galaxy NGC 4302 Revealed by the Atacama Large Millimeter/submillimeter Array
Authors: Kijeong Yim, Tony Wong, Richard J. Rand
Figure caption: Left: radial surface density profiles of H2 (red squares), H I (blue circles), SFR (magenta diamonds), and the total gas (black triangles). The vertical error bars represent the standard deviation of data in a radial bin. Right: SFR radial profiles from the linear combination of Hα and 24 μm (magenta diamonds) and the radio continuum (blue circles). The vertical error bars are the standard deviation of the average in each bin of 25″.
Paper: The Volumetric Star Formation Law in the Almost Edge-on Galaxy NGC 4302 Revealed by the Atacama Large Millimeter/submillimeter Array
Authors: Kijeong Yim, Tony Wong, Richard J. Rand
Figure caption: Scale heights of H I (blue circles) and CO (red squares) as functions of radius. The open (blueshifted side) and filled (redshifted side) circles are average values in bins of 3″ (CO) and 7″ (H I). The lines are the linear least-squares fit to the average data points. The shaded regions around the best fit lines show uncertainties of the best fits and the vertical error bars show uncertainties of the Gaussian fitting for the scale height. The right three panels show Gaussian fits (line) to the vertical profiles (filled circles) of CO at x-offsets of −34″, 56″, and 78″.
Paper: The Volumetric Star Formation Law in the Almost Edge-on Galaxy NGC 4302 Revealed by the Atacama Large Millimeter/submillimeter Array
Authors: Kijeong Yim, Tony Wong, Richard J. Rand
Figure caption: Top panels: SFR volume density ρ SFR as a function of ρ HI (blue circles), ﹩{\rho }_{{{\rm{H}}}_{2}}﹩ (red squares), and ρ gas (black triangles). SFR surface density ΣSFR as a function ΣH I, ﹩{{\rm{\Sigma }}}_{{{\rm{H}}}_{2}}﹩, and Σgas. The gas depletion time (SFE−1) is labeled on the corresponding dashed lines. Bottom panels: H2, H I, and the total gas SFEs as a function of radius for volume (left) and surface (right) densities. The vertical error bars represent the standard deviation of data in each bin.
Paper: A Search for Lensed Lyα Emitters within the Early HETDEX Data Set
Authors: Isaac H. Laseter, Steven L. Finkelstein, Micaela J. Bagley, Dustin M. Davis, Karl Gebhardt, Caryl Gronwall, Robin Ciardullo, Gregory R. Zeimann, Erin Mentuch Cooper, Daniel Farrow
Figure caption: Returned HETDEX fibers, emission-line fit, best available imaging of foreground source, and complete spectrum for the potential LAE lensed system rediscovered from Shu et al. (2016). The overall returned plots originate from ELiXer, which is discussed in detail in Section 3.2. As stated before, we are in agreement with the determined redshift found by Shu et al. (2016). Top Left: Two best VIRUS fibers, pixel flats, smoothed VIRUS fibers, and weighted sum of fibers. The information on the sides of the fibers can be summarized as technical observation/pipeline information. The information on the right specifies the emission line on the CCD and the dither/shot information. The information on the left specifies the position of the fiber on the CCD and the fit to the expected fiber profile. Top Middle: Gaussian fit to emission line with wavelength given in Å and flux given in erg s−1 cm−2 over a 2 Å window. Top Right: Best available imaging at the location of lensed LAE candidate, which for this case is with the Hyper Suprime-Cam r band with the limited magnitude given. The panel distances are given in arcseconds. Bottom: Full VIRUS spectrum of the potential lensed LAE system from Shu et al. (2016). Plotted is flux given in erg s−1 cm−2 over a 2 Å bin vs. wavelength given in Å. The yellow box with a dashed line denotes the location of the identified potential Lyα. The width of the yellow box is equal to the width of the Gaussian cutout plot. The two gray columns represent skylines. The extra dashed lines and highlight colors indicate possible emission or absorption lines that pass a certain threshold from ELiXer. These are automatic in the ELiXer pipeline, but are not used for the analysis of this work, as we are concerned with background LAE emission (see Section 3.2). The gray shaded region in the 1D spectra is a “rough” estimate of noise, not uncertainties on the flux measurement. The regions come from the standard deviation of flux per wavelength bin for a few hundred fibers spatially near the fibers of the detection (sigma clipping mostly excludes fibers that have significant signal from objects). Therefore, the fibers utilized for the standard deviation are mostly (but not strictly) sky fibers. The gray regions act only as a visual cue to the user, but are not otherwise used in any calculation. For faint emission lines, they can be very near this “noise.”
Paper: A Search for Lensed Lyα Emitters within the Early HETDEX Data Set
Authors: Isaac H. Laseter, Steven L. Finkelstein, Micaela J. Bagley, Dustin M. Davis, Karl Gebhardt, Caryl Gronwall, Robin Ciardullo, Gregory R. Zeimann, Erin Mentuch Cooper, Daniel Farrow
Figure caption: Best available imaging for the gravitationally lensed LAE candidates. We present the background lens redshift, magnification determined in Section 4, and the limiting magnitudes of each image, which are reported from the surveys themselves and are survey-wide averages (See Section 2.1). The crosshair of each image focuses on the center of the background LAE candidate position, which is determined from the spectroscopic detection in the HETDEX spectral database found from ELiXer. The values along each axis represent arcseconds away from the central position of the image. The red box represents a ±3″ distance from the center of the image. The overlaid circles represent VIRUS fiber locations, with the colors blue, green, orange, and red representing the fiber weights from strongest to weakest. The imagining was taken directly from ELiXer, which has automatic contrast stretching, i.e., the bright foreground lens causes a poor stretch for identifying fainter regions. Moreover, due to the limited sensitivity of the best available imaging, the background LAE candidates being exceedingly faint, and the foreground object being bright, we do not expect a counterpart to the gravitationally lensed LAE location to be apparent in the current imaging. Nonetheless, the imaging is important to the current work, as the magnification determination (Section 4) requires distances between the foreground lens and the background LAE candidate. With deeper imaging, we expect for a counterpart to the Lyα detection to be discernible. The HSC-r imaging is customized for the HETDEX survey and is not associated with the Subaru Strategic Program.
Paper: A Search for Lensed Lyα Emitters within the Early HETDEX Data Set
Authors: Isaac H. Laseter, Steven L. Finkelstein, Micaela J. Bagley, Dustin M. Davis, Karl Gebhardt, Caryl Gronwall, Robin Ciardullo, Gregory R. Zeimann, Erin Mentuch Cooper, Daniel Farrow
Figure caption: Example of neighborhood spectra returned using a 5″ search radius from the foreground galaxy's position using ELiXer for object 20190325v015-9900150001. The first two spectra are oriented on the foreground galaxy and contain a nondetection (red line in top spectrum) and an [O II] emission (red line in second spectrum), respectively. The third spectrum is 4.″2 away from the foreground galaxy and contains an emission line not present in the foreground galaxy spectrum and not originating from the foreground galaxy (z lens = 0.4340, λ = 3772.96 Å, λ 0 = 2631.07 Å). We thus consider this detection a possible potential lensed LAE. The fourth spectrum, although containing an emission line, is 9.″8 away from the foreground galaxy, and we thus do not consider it a viable potential lensed LAE. For each image panel, the distances are given in arcseconds. For each spectrum, the flux is given in units of f λ  = 1 × 10−17 erg s−1 cm−2. The gray dashed line at 3675.83Å present in each spectrum represents ELiXer’s first extraction of the region. In this case, the first extraction is a nondetection, but the wavelength of the first extraction is represented in the subsequent spectra. The red dashed line is the line for each detection corresponding to the red box in the associated imaging to the left. The neighbor search with ELiXer simply finds detections in the HETDEX detection catalog, so if a neighboring detection is on the same initial object, one would expect to see the gray dashed line and the red line overlap (e.g., the top spectrum), or if an object has multiple detections, the other detection would show up as a “neighbor” (e.g., the second spectrum).
Paper: A Search for Lensed Lyα Emitters within the Early HETDEX Data Set
Authors: Isaac H. Laseter, Steven L. Finkelstein, Micaela J. Bagley, Dustin M. Davis, Karl Gebhardt, Caryl Gronwall, Robin Ciardullo, Gregory R. Zeimann, Erin Mentuch Cooper, Daniel Farrow
Figure caption: R.A.: 167.706955 (ICRS, deg), decl.: 51.316486 (ICRS, deg). Same layout as described in Figure 1. The red and green labels and the respective identifications above the 1D spectrum represent potential locations of emission/absorption lines if the identified line is either Lyα or [O II]. In this case no potential secondary line is seen, though this is nearly always the case when the primary line is identified as Lyα. As described in Section 3.3, the spectroscopic redshift of the foreground galaxy is z  ls  = 0.4483, with the identified emission line having λ = 4281.26 Å, which would make the identified emission line have a rest-frame wavelength of 2956.06Å. The closest neighboring rest-frame emission lines are He I λ2945.11 and O III λ3132.79.