adsabs/AstroCLIMB huggingface dataset:
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Unfolded spectrum and best-fit model for NGC 3982. Black denotes Chandra data of the AGN core. Red and green denote FPMA and FPMB data from the NuSTAR observation of NGC3982. The Chandra data of Src 1 are depicted in light gray.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Chandra and NuSTAR FPMA images of NGC 3982. The larger, 40″ radius circle denotes the NuSTAR extraction region, while the smaller circles denote the Chandra extraction regions. An off-nuclear point source (Src 1) is visible in the Chandra image, and it was bright enough that it had to be accounted for in the spectral fitting.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Chandra and NuSTAR FPMA images of IC 3639. The larger, 40″ radius circle denotes the NuSTAR extraction region, while the smaller circles denote the Chandra extraction regions. An off-nuclear point source (Src 1) is visible in the Chandra image, but is sufficiently faint to be ignored in the X-ray spectral fitting.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Unfolded spectrum and best-fit model for IC 3639. Black denotes Chandra data, green denotes NuSTAR FPMA data, and red denotes NuSTAR FPMB data.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Unfolded spectrum and best-fit model for NGC 3627. Black denotes Chandra data and model for the AGN core. Red and green denote NuSTAR FPMA and FPMB data and models. The Chandra data and models for the off-nuclear sources are depicted in light gray.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Chandra (ObsID: 15065) and NuSTAR FPMA images of NGC 4922. The larger, 40″ radius circle denotes the NuSTAR extraction region, while the smaller circle denotes the Chandra extraction region.
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: The effect of incorporating uncertainties in logM* and logSFR on the inferred density, P(logSFR∣logM *, z). The top panel shows the joint logM*–logSFR posterior for a single object, demonstrating that increasing the number of posterior samples for one object produces a better resolution in both the 1D uncertainties for mass and star formation rate, and of the correlation between them. The lower panels show the density profile across the star-forming sequence at fixed M * and redshift. The colors in each panel denote how many posterior samples were included from each galaxy when inferring the density in (logM*, logSFR, z) with the normalizing flow method. The ridge of the star-forming sequence is marked with a dashed line. Including uncertainties has a relatively strong effect on the profile of the sequence at high masses, shifting the median by ∼0.2 dex. This sensitivity arises because the uncertainty on the average star formation rate is relatively high due to the larger number of low-sSFR systems, and the number of objects is relatively low. In contrast, measurement uncertainty has a relatively negligible effect on lower mass systems, likely due to the fact that they are far more numerous due to the shape of the galaxy stellar mass function.
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: Four different methods to select star-forming galaxies, and the properties of the resulting star-forming sequences. The top panels show the SFR–M* plane for galaxies at 0.3 < z < 0.7 identified as star-forming via four different techniques, with the total number of objects included in the fit indicated in the upper left and the mean and 1σ scatter of the resulting star-forming sequence as solid and dashed lines, respectively. For the Gaussian mixture model, the quiescent sequence is also shown. The lower panels show the median and 1σ width of the resulting star-forming sequence and the fraction of quiescent galaxies inferred from each method. For reference, we additionally show the values derived later in this paper with a gray dashed line.
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: Slices of the log SFR distribution at fixed values of logM* and redshift from the density estimate are in black, while Gaussian fits to the star-forming sequence shown in red. The fit is performed iteratively using sigma-clipping with a variable lower bound as described in the text. The fit limit in each panel is indicated with a dashed line. The stellar mass and redshift of each panel are indicated in the upper left, along with the inferred width of the star-forming sequence. There is a fundamental trade-off between the fidelity of the Gaussian fit to the high-SFR end of the distribution and the exclusion of the long tail of quenching or quiescent galaxies below the star-forming sequence.
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: The evolution of parameters derived from ﹩\rho (\mathrm{logSFR}\,| \mathrm{log}{M}^{* },z)﹩. In order of left to right, the first row shows the mean SFR, the ridge of the star-forming sequence, and the slope of the ridge, while the second row shows the quiescent fraction, the 1σ width of the star-forming sequence in logSFR, and the 1σ width in logSFR of the full population. The slope of the ridge is clipped at 0 to avoid having the color scale dominated by the down-turn at high masses and low redshifts. The parameter maps are smoothed with Gaussian kernels with width δ z = 0.1, δlog M* = 0.1 for presentation purposes.
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: The redshift evolution of the low- and high-mass slope and the stellar mass at which the slope transitions between the two. The high- and low-mass slopes are distinct at all redshifts. However, the need for multiple slopes in the ridge of the star-forming sequence is most clear at low redshifts. This is because at higher redshifts the transition mass increases to higher values of stellar mass, at which there are few (N ∼ 5–10, see, Figure 1 in Leja et al. 2020) observable galaxies in these fields, meaning both the mean and ridgeline SFRs are more weakly constrained.
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: The log M*–logSFR relationship at six redshifts. The color shading indicates the log-density ﹩\mathrm{log}\rho (\mathrm{log}{M}^{* },\mathrm{logSFR},{\text{}}z)﹩ estimated from our normalizing flow. The thick teal line shows the running median, with the thin teal lines showing the 16th/84th percentiles. The dashed blue line shows the mode (i.e., the ridgeline), while the dashed–dotted red line shows the mean SFR (as opposed to the mean logSFR). Below z = 0.5, the mass-complete limit is from COSMOS-2015, while above z = 0.5 it is from the deeper 3D-HST survey.
Paper: A New Census of the 0.2 < z < 3.0 Universe. II. The Star-forming Sequence
Authors: Joel Leja, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Benjamin D. Johnson, Charlie Conroy, Katherine E. Whitaker, Erica J. Nelson, Pieter van Dokkum, Marijn Franx
Figure caption: The left panel shows the evolution of the ridge of the star-forming sequence while the right panel shows the evolution of the mean SFR. The mean SFR includes contributions from both star-forming and quiescent galaxies. The points are measurements from the density field evaluated using the normalizing flow. The lines show the broken power-law fits described in Equations (9) and (10).
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Unfolded spectrum and model for the ultraluminous X-ray source M66 X-1, which was observed along with NGC 3627. Black denotes Chandra data, while red and green represent NuSTAR FPMA and FPMB data, respectively.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Illustration of the baryonic subcycling and what physical quantities are available within A-SLOTH. Top: various mass contents along one merger tree branch as a function of time after the big bang. Bottom: gas metallicity of the IGM (blue) and ISM (black). The illustrated time corresponds to the redshift range z = 27 − 18. We witness the formation of the first Pop III stars around 110 Myr (orange), the suppression of further star formation by SNe around 120 Myr (olive), the accumulation of further cold gas around 130 Myr (blue), and the formation of second-generation stars after ∼140 Myr (cyan). The ISM metallicity experiences strong variations during the first SN explosions. This is due to the small amount of residual gas and metals that remain in the halo. The new stellar mass δ M * (purple) and the ejected metal mass δ M metals (olive) are the instantaneous values at the specific time step during subcycling. The halo mass M halo (green) increases in steps, which illustrates the original redshift steps from the merger tree. The stellar masses (orange, cyan) and outflow mass (pink) are cumulative and therefore monotonically increasing.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Ionization history simulated with A-SLOTH (blue), compared to various models (dashed) and observations (points).
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Illustration of SN energy, ionizing photon production rate, carbon and iron ejecta mass, and stellar lifetimes that are available as input data in A-SLOTH. Pop III stars are plotted in red, and Pop II stars are plotted in blue. Users can define their own specific mass ranges or use other tabulated input data.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Illustration of the spatial extent of external feedback at z = 6. We show the fraction of ionized volume along lines of sight in orange, the average IGM metallicity along lines of sight in blue, and halos with M vir > 4 × 108 M ⊙ as black circles.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption:  A-SLOTH conquering a merger tree.
Paper: An EUV Jet Driven by a Series of Transition Region Microjets
Authors: Hengyuan Wei, Zhenghua Huang, Hui Fu, Ming Xiong, Lidong Xia, Chao Zhang, Kaiwen Deng, Haiyi Li
Figure caption: Spacetime plots along the trajectory of the EUV jet (see the green diamond symbols in Figure 1(a)) taken from IRIS SJ 1400 Å images (a), AIA 171 Å (b), and AIA 94 Å (c). The apparent speeds derived from these plots are also marked.
Paper: Observations of Thomson Scattering from a Loop-prominence System
Authors: Juan Carlos Martínez Oliveros, Juan Camilo Guevara Gómez, Pascal Saint-Hilaire, Hugh Hudson, Säm Krucker
Figure caption: Left: the “loci plot” comparing the microwave emission measure with X-rays. The GOES and RHESSI exclusion lines agree well with the RHESSI 12–18 keV flux, and match the short-wavelength extrapolation of the microwave thermal flux. Right (Section 4): constraints on the mean source density for the polarization source, combining HMI observations with X-ray and microwave data. The colored lines at the top are limits imposed by the Razin–Tsytovich effect (red) and by free–free opacity (blue), in the absence of a long-wavelength spectral break (e.g., Belkora 1996). The heavy black line corresponds to filling factory unity, with the thin lines for values of 0.3 and 0.1. The vertical dashed lines are the box A width times 0.5, 1, and 2.
Paper: Observations of Thomson Scattering from a Loop-prominence System
Authors: Juan Carlos Martínez Oliveros, Juan Camilo Guevara Gómez, Pascal Saint-Hilaire, Hugh Hudson, Säm Krucker
Figure caption: Top left and right panels show the column densities for regions A and B, respectively, the shadow refers to the errors in each case. In both cases, the dashed curve is the column density without correction by the polarization factor whereas the solid and shadowed region have the correction done. The bottom panels are the densities for the regions A and B derived from the column densities assuming a line-of-sight thickness between 2.9 and 40.7 Mm (shadowed regions).
Paper: Observations of Thomson Scattering from a Loop-prominence System
Authors: Juan Carlos Martínez Oliveros, Juan Camilo Guevara Gómez, Pascal Saint-Hilaire, Hugh Hudson, Säm Krucker
Figure caption: Single-frequency observations of SOL 2017-09-10 from RSTN/San Vito (4.995, 8.8, and 15.4 GHz), with preevent background levels subtracted. The minimum coincides approximately with the box A snapshot time. The radio spectral irradiances are measured in standard solar flux units, 10−22 W (m2 Hz)−1.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: (a) Distribution of the SO2 integrated emission in the space of radius from ALMA source 2 and polar angle. The yellow star marks the location of source 4. For each radius between 0.″2 and 0.″8 where the spiral structures can be well defined, the polar angles of the emission peaks of the two spirals are determined (data points). The errors(shown in 3σ levels) are determined by the beam size, radius, and the S/N, following Δθ = θ beam/(2r S/N), where θ beam = 0.″3 and r is the radius (distance to source 2). (b) Fits to the spiral structures in the SO2 integrated emission map around ALMA source 2. The polar angle of the SE arm is rotated by 180° to compare with the NW arm. Each spiral structure is fitted with a logarithmic spiral (red curve) and an Archimedean spiral (blue curve).
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: Integrated intensity maps of different emission lines (color scale and gray contours) overlaid with the 1.3 mm continuum emission (blue contours). The molecule names and integrated V lsr ranges are labeled in each panel. The continuum contour levels are at 10σ × 2 n  (1σ = 0.48 mJy beam−1, n = 0, 1, …). The line emission contours have the lowest level and intervals of 3σ, with 1σ = 8.3, 7.6, 12.5, 7.3, 8.0, and 7.2 K km s−1 in panels (a)–(f), respectively. The yellow stars mark the positions of sources 1, 2, and 4 identified from the C9 configuration data (source names are labeled in panel (a)). The red curve shows the spiral structure fitted from the SO2 integrated map.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: (a) The continuum SED of source 1 for VLA bands and ALMA 1.3 mm continuum (data points). The red dashed line shows the free–free emission of the best-fit model. The blue dashed line shows the dust emission of the best-fit model. The black dashed line shows the total continuum emission. The inset panel shows the 3σ level of the H30α integrated map used as the upper limit (red data point) and the model prediction (red dashed line). (b)−(e) χ 2 distribution with model parameters: electron temperature T  e  (panel (b)), the emission measure EM0 at the radius of 10 au (panel (c)), the power-law index of the emission measure distribution ρ EM (panel (d)), and the spectral index of the dust component α dust (panel (e)). (f) χ 2 distribution with the ionizing photon rate ﹩{\dot{N}}_{{\rm{i}}}﹩ calculated from T  e , EM0, and ρ EM.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: PV diagrams of the (a) SO2, (b) H2CO, (c) CH3OH, (d) SiO, (e) H2S, and (f) CH3OCH3 emissions around source 2 along a cut with a position angle of P.A. = −25°, i.e., the disk orientation obtained from the fit done by Sánchez-Monge et al. (2013), shown in color scales and black contours. The position offset is relative to the continuum peak position of source 2 identified from the C9 configuration data. The horizontal line indicates the systemic velocity of V sys = 30 km s−1 of the source, The contours have the lowest level and intervals of 3σ, with 1σ = 3.2, 3.7, 4.5, 3.3, 3.2, and 2.6 mJy beam−1 in panels (a)–(f), respectively.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: Channel maps of the SO2 (222,20 − 221,21) emission (color scale and gray contours). The central velocity of each channel is labeled in each panel. The gray contours start at 3σ and have intervals of 6σ (1σ = 3.3 mJy beam−1). The black contours show the continuum emission (same as Figure 12). The yellow stars mark the positions of sources 1, 2, and 4 identified from the C9 configuration data (source names are labeled in the top-left panel). The red curve shows the spiral structure fitted from the SO2 integrated map. The synthesized beam is shown in the lower-left corner of each panel.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: (a) Moment 1 map of the SO2 (222,20 − 221,21) emission shown in color scale, overlaid by the continuum emission shown in gray contours. The three stars mark the positions of sources 1, 4, and 2. The square indicates the region shown in panel (b). (b) same as panel (a), but for the CH3OH (42,2 − 31,2; E) line. (c) A zoom-in view of the moment 1 map of the SO2 emission around source 1 (marked with the star). Data combining C3, C6, and C9 configurations are used. (d) Same as panel (c), but for the CH3OH (42,2 − 31,2; E) line.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: Same as Figure 8, but for ALMA source 3. As the H30α line in this source has a potential maser component, we use it as an upper limit to constrain the model (inset of panel (a)).
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: Same as Figure 13, but for the CH3OH (42,2 − 31,2; E) line. The gray contours start at 3σ and have intervals of 6σ (1σ = 3.7 mJy beam−1).
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: Same as Figure 8, but for ALMA source 4. The 6 cm flux is also not used in the fitting (see the text).