adsabs/AstroCLIMB huggingface dataset:
Paper: Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744
Authors: Katherine A. Suess, John R. Weaver, Sedona H. Price, Richard Pan, Bingjie Wang, 冰洁 王, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Ivo Labbé, Joel Leja, Christina C. Williams, Katherine E. Whitaker, Hakim Atek, Pratika Dayal, Anna de Graaff, Robert Feldmann, Marijn Franx, Yoshinobu Fudamoto, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Jenny E. Greene, Gourav Khullar, Vasily Kokorev, Mariska Kriek, Brian Lorenz, Danilo Marchesini, Michael V. Maseda, Jorryt Matthee, Tim B. Miller, Ikki Mitsuhashi, Lamiya A. Mowla, Adam Muzzin, Rohan P. Naidu, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, David J. Setton, Heath Shipley, Renske Smit, Justin S. Spilker, Pieter van Dokkum, Adi Zitrin
Figure caption: Existing photometric coverage in both the NIRCam primary and NIRISS parallel fields, along with new imaging from this program. MegaScience “completes” the imaging in the primary field, with deep images in all 20 of NIRCam’s broad- and medium-band filters. The addition of two broadband and four medium-band filters in the NIRISS parallel field will allow for robust SED modeling.
Paper: Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744
Authors: Katherine A. Suess, John R. Weaver, Sedona H. Price, Richard Pan, Bingjie Wang, 冰洁 王, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Ivo Labbé, Joel Leja, Christina C. Williams, Katherine E. Whitaker, Hakim Atek, Pratika Dayal, Anna de Graaff, Robert Feldmann, Marijn Franx, Yoshinobu Fudamoto, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Jenny E. Greene, Gourav Khullar, Vasily Kokorev, Mariska Kriek, Brian Lorenz, Danilo Marchesini, Michael V. Maseda, Jorryt Matthee, Tim B. Miller, Ikki Mitsuhashi, Lamiya A. Mowla, Adam Muzzin, Rohan P. Naidu, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, David J. Setton, Heath Shipley, Renske Smit, Justin S. Spilker, Pieter van Dokkum, Adi Zitrin
Figure caption: Spectral features probed by our primary medium-band observations as a function of redshift.
Paper: Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744
Authors: Katherine A. Suess, John R. Weaver, Sedona H. Price, Richard Pan, Bingjie Wang, 冰洁 王, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Ivo Labbé, Joel Leja, Christina C. Williams, Katherine E. Whitaker, Hakim Atek, Pratika Dayal, Anna de Graaff, Robert Feldmann, Marijn Franx, Yoshinobu Fudamoto, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Jenny E. Greene, Gourav Khullar, Vasily Kokorev, Mariska Kriek, Brian Lorenz, Danilo Marchesini, Michael V. Maseda, Jorryt Matthee, Tim B. Miller, Ikki Mitsuhashi, Lamiya A. Mowla, Adam Muzzin, Rohan P. Naidu, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, David J. Setton, Heath Shipley, Renske Smit, Justin S. Spilker, Pieter van Dokkum, Adi Zitrin
Figure caption: Example of galaxies at cosmic morning, 3 ≲ z ≲ 6. Color images are shown on a linear stretch; the white scale bar shows 0.″5; emission lines are labeled with red, green, or blue text, depending on which filter they are expected to fall into.
Paper: Measurements of the Reaction Rate Coefficients of Atomic Hydrogen with Astrochemical Anions: CN− and C3N− 
Authors: Christine Lochmann, Sruthi Purushu Melath, Robert Wild, Ersin Yurtsever, Alberto Martín Santa Daría, Lola González-Sánchez, Francesco A. Gianturco, Roland Wester
Figure caption: Temperature-dependent Cl− loss rate from the trap due to reactions with H atoms and H atom density. There are three calibration regions depending on the recombination of H to H2: region I from 290 to 70 K (points), region II from 65 to 30 K (triangles), and region III at 7 K (diamonds). The solid purple line shows the 1/﹩\sqrt{T}﹩ dependence of the chlorine loss rate, which may include the temperature dependence of the H + Cl− cross section as well as the decreasing velocity of the H atoms due to the cooling. The solid dark gray line shows the linear fit for region II.
Paper: Measurements of the Reaction Rate Coefficients of Atomic Hydrogen with Astrochemical Anions: CN− and C3N− 
Authors: Christine Lochmann, Sruthi Purushu Melath, Robert Wild, Ersin Yurtsever, Alberto Martín Santa Daría, Lola González-Sánchez, Francesco A. Gianturco, Roland Wester
Figure caption: Temperature-dependent reaction rate coefficient of C3N− with atomic hydrogen. The symbols, corresponding to the different calibration regions, follow the same formatting as discussed in Section 3. The thermal rate coefficient, as measured by Z. Yang et al. (2011), is shown as an orange star. The solid line is the temperature-dependent rate coefficient as determined by a power-law fit. The dashed line represents the Langevin capture rate coefficient.
Paper: Measurements of the Reaction Rate Coefficients of Atomic Hydrogen with Astrochemical Anions: CN− and C3N− 
Authors: Christine Lochmann, Sruthi Purushu Melath, Robert Wild, Ersin Yurtsever, Alberto Martín Santa Daría, Lola González-Sánchez, Francesco A. Gianturco, Roland Wester
Figure caption: Example of the evolution of the trapped ion number in the trap at a temperature of 90 K. The solid points denote the C3N− ion signal after interaction with H atoms. The circles denote the background ion signal. The red line is an exponential decay fit to extract the ion loss rate after interaction with H atoms. The black line shows an exponential fit to the background, which yields a lifetime of more than 1000 s.
Paper: Reverberation Mapping of High-mass and High-redshift Quasars Using Gravitational Time Delays
Authors: Miriam Golubchik, Charles L. Steinhardt, Adi Zitrin, Ashish K. Meena, Lukas J. Furtak, Doron Chelouche, Shai Kaspi
Figure caption: Overlap of the distribution of SL TDs by lensing clusters, and the distribution of expected RM time lags from the BLR sizes for different redshifts. We show the distribution for both high- and low-mass galaxy clusters. The redshift limits in each panel’s legend indicate the redshift range of the sources that are lensed to create the SL TD distribution. The RM time lags are corrected for the specified, central redshift, i.e., they are given in the observed frame as well. As can be seen, there is substantial overlap such that SL TDs by galaxy clusters completely cover the range of expected RM lag times. We also mark with a dashed black line a typical TD caused by galaxy–galaxy SL by a massive galaxy (where we adopt a singular isothermal sphere (SIS) galaxy model with σ = 250 km s−1 placed at z = 0.5), showing that only galaxy clusters supply large enough TDs for our purpose. As can be seen, smaller galaxy cluster lenses show more overlap, but they are also expected to show fewer multiple images per cluster. For more details see Section 2.
Paper: Reverberation Mapping of High-mass and High-redshift Quasars Using Gravitational Time Delays
Authors: Miriam Golubchik, Charles L. Steinhardt, Adi Zitrin, Ashish K. Meena, Lukas J. Furtak, Doron Chelouche, Shai Kaspi
Figure caption: Histograms of the expected BLR sizes for SDSS DR7 quasars. The catalog contains two distinct subsamples (see Section 2.1 for details). The Hβ RM time-lag distribution is plotted for the subsample of quasars which have an optical continuum measurement, assuming the R–L relation by M. C. Bentz et al. (2013). The C IV time-lag distribution is plotted for the subsample of quasars which have a UV continuum measurement, using the relation from S. Kaspi et al. (2021). The distributions seem to each fit well with a Gaussian distribution, with [μ, σ] = [1.86, 0.21] and [μ, σ] = [1.78, 0.16] for Hβ and C IV, respectively. For example, ∼9% (∼26%) of the expected C IV (Hβ) rest-frame RM time lags will be 100 days or longer. This means 500−1300 observed days, depending on redshift. The reader should also note that in general, for the same quasar, the Hβ RM time lags are expected to be longer by a factor of a few compared to the C IV RM time lags, so that in practice the Hβ distribution may extend to even longer RM time lags.
Paper: Reverberation Mapping of High-mass and High-redshift Quasars Using Gravitational Time Delays
Authors: Miriam Golubchik, Charles L. Steinhardt, Adi Zitrin, Ashish K. Meena, Lukas J. Furtak, Doron Chelouche, Shai Kaspi
Figure caption: Simulated idealized light curve for the case where the TD equals the RM time lag. In the top panel of the figure we demonstrate mock light curves of two images of the same source. The x-axis represents the observing time of the images and the y-axis represents the normalized flux. The SL TD between the two images is 1000 days, where image A is the trailing image and image B is the leading image. The orange and blue curves correspond to the mock continuum and emission-line light curves, respectively. Since the two images will have different magnification factors, the leading image shown in the top right panel has its flux normalized lower, as it will usually have a lower magnification than the trailing one. Details on the mock data are given in Section 5.1. In the bottom panel we show the full mock light curves with shaded areas emphasizing the data obtained from each image and the overlap. The mock light curves of the leading image B are corrected by the TD. We emphasize the RM time lag between the continuum and emission curves at several points with arrows.
Paper: Measurements of the Reaction Rate Coefficients of Atomic Hydrogen with Astrochemical Anions: CN− and C3N− 
Authors: Christine Lochmann, Sruthi Purushu Melath, Robert Wild, Ersin Yurtsever, Alberto Martín Santa Daría, Lola González-Sánchez, Francesco A. Gianturco, Roland Wester
Figure caption: Interaction potentials, in Jacobi coordinates, for the different angles of approach of the H atom to CN− (left panel) and C3N− (right panel). An approach on the N-terminated side of the molecules corresponds to an angle of 0°, whereas the approach on the C-terminated side corresponds to an angle of 180°. The vertical dashed lines denote the average distance below which the AD process can occur because of curve crossings with neutral potential curves (not shown). Depending on the angle, this distance varies by about 1 Å. For C3N−, it is visible that a barrier is only found for a more limited range of angles than for CN−. The barriers’ locations vary from about 2.5 to about 3.5 Å.
Paper: Reverberation Mapping of High-mass and High-redshift Quasars Using Gravitational Time Delays
Authors: Miriam Golubchik, Charles L. Steinhardt, Adi Zitrin, Ashish K. Meena, Lukas J. Furtak, Doron Chelouche, Shai Kaspi
Figure caption: Histogram of the redshift of the two subsamples of SDSS DR7 quasars used to construct the distributions in Figure 1. The AGNs used to construct the Hβ RM time-lag distribution are all at redshift < 1 with a median redshift of 0.59. As for the quasars used to construct the C IV RM time-lag distribution, 80% are between redshifts 1.5 and 2.5, with a median redshift of 1.9.
Paper: Measurements of the Reaction Rate Coefficients of Atomic Hydrogen with Astrochemical Anions: CN− and C3N− 
Authors: Christine Lochmann, Sruthi Purushu Melath, Robert Wild, Ersin Yurtsever, Alberto Martín Santa Daría, Lola González-Sánchez, Francesco A. Gianturco, Roland Wester
Figure caption: Temperature-dependent rate coefficient of the reaction of CN− with H atoms. The symbols correspond to the different calibration regions, as discussed in Section 3. The orange star represents the thermal rate coefficient previously measured by Z. Yang et al. (2011) at 298 K. The light blue line is the temperature-dependent rate coefficient below 160 K,as determined by a power-law fit. The dashed line represents the Langevin capture rate coefficient.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Best-fit model of the gaseous CO rovibrational absorption lines in IR08572 NW. The abscissa is the rest wavelength. The ordinate is the normalized flux. Components (a)–(e) and their sum are denoted in red, orange, green, dark-blue, pink, and sky-blue lines, respectively. Black arrows denote the rest wavelength of each CO transition. The emission lines of HI Pfβ and H2 v = 0 → 0 S(9) are colored olive-green. Ice features of H2O, ﹩{\mathrm{OCN}}^{-}﹩, CO, and OCS are denoted with solid gray lines. Note that the results of our velocity decomposition for IR08572 NW are slightly different from those in S. Onishi et al. (2021). This occurred because we consider the emission lines of HI Pfβ and H2 v = 0 → 0 S(9) in the model fitting in this paper, as well as the gaseous CO absorption lines, whereas S. Onishi et al. (2021) excluded the emission lines in the continuum-normalization step before the fitting.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Best-fit model of the gaseous CO rovibrational absorption lines in N4418. The abscissa is the rest wavelength. The ordinate is the normalized flux. Components (a) and (b) and their sum are denoted with red, orange, and sky-blue lines, respectively. In addition, component (b) of 13CO absorption lines are shown with orange dashed lines. The black arrows denote the rest wavelength of each CO transition. The HI Pfβ and the H2 v = 0 → 0 S(9) emission line are colored olive-green.
Paper: A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Francesca Capel, Julian Kuhlmann, Christian Haack, Martin Ha Minh, Hans Niederhausen, Lisa Schumacher
Figure caption: Summary of the likelihood for point-source components. Open and shaded circles are used to show model parameters and fixed observables, respectively, with the arrows showing the connections between them. The boxes are used to separate the N s source components and n  ν  events. The parameters are explained in the text. The levels, from upper to lower, show the source properties, latent or “hidden” true parameters that depend on the source properties and cannot be directly observed, and observable quantities that depend on the IRF. The latent source labels, λ  i , are discrete parameters marking the mixture model component that each event belongs to.
Paper: A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Francesca Capel, Julian Kuhlmann, Christian Haack, Martin Ha Minh, Hans Niederhausen, Lisa Schumacher
Figure caption: Upper panel: the differentital flux normalization at 1 TeV for simulated point sources. The SkyLLH sensitivity assuming an E −2 power-law spectrum as reported in C. Bellenghi et al. (2023a) is shown for comparison, as this calculation makes use of the same publicly available IRF that is used here. We also plot an estimation of the discovery potential by rescaling the sensitivity as a function of decl. This rescaling is calculated as the ratio of the discovery potential to the sensitivity, according to the results presented in M. G. Aartsen et al. (2020), which are also shown for comparison. Lower panel: the total expected number of neutrino events for simulated point sources is shown in comparison to that required by the sensitivity and discovery potential curves introduced above.
Paper: A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Francesca Capel, Julian Kuhlmann, Christian Haack, Martin Ha Minh, Hans Niederhausen, Lisa Schumacher
Figure caption: Color-coded posterior association probabilities of events to source #1. Left panel: spatial distribution of events. The marker size does not represent the angular resolution and the point-source events are highlighted in red borders. Right panel: marginal posteriors for the true neutrino energies of events included in the ROI. Markers on the top row indicate ﹩\hat{E}﹩ for all events included in the analysis, with dashed connecting lines to the posteriors for the events from the tested point source.
Paper: A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Francesca Capel, Julian Kuhlmann, Christian Haack, Martin Ha Minh, Hans Niederhausen, Lisa Schumacher
Figure caption: The simulated data set containing 669,007 events with ﹩\hat{E}\gt 300﹩ GeV. The left panel shows a sky map of the event directions with the selected source positions overlaid. The right panel shows the distribution of events in ﹩\hat{E}﹩ and ﹩\sin (\delta )﹩; see Figure 1 in IceCube Collaboration (2021).
Paper: A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Francesca Capel, Julian Kuhlmann, Christian Haack, Martin Ha Minh, Hans Niederhausen, Lisa Schumacher
Figure caption: Marginal posterior density of the expected number of point-source events for source #1, ﹩{\bar{n}}_{1}﹩. The number of selected source events in each fit is color-coded, with n 1 = [0, 5, 10, 14] shown.
Paper: A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Francesca Capel, Julian Kuhlmann, Christian Haack, Martin Ha Minh, Hans Niederhausen, Lisa Schumacher
Figure caption: The joint posterior density of L and γ s with contours showing the 30%, 60%, and 90% HDIs. The true parameter values are indicated by the horizontal and vertical solid lines. The upper and right panels show the marginal distributions in comparison with the prior.
Paper: Bright in the Black: Searching for Electromagnetic Counterparts to Gravitational-wave Candidates in LIGO-Virgo-KAGRA Observation Runs with AstroSat-CZTI
Authors: Gaurav Waratkar, Varun Bhalerao, Dipankar Bhattacharya
Figure caption: Comparison of limits on derived isotropic luminosities for the three events in our GW event sample that contain a neutron star, as discussed in Section 4.1. All values are scaled to the 1 keV–10 MeV band. The downward pointing triangles mark the limits on source luminosity at the median distance of these events as given in The LIGO Scientific Collaboration et al. (2021), using AstroSat-CZTI flux upper limits calculated in Section 2.2 for the three time bins: 0.1 s (green), 1.0 s (red), and 10.0 s (purple). The shaded inclined bands show the limits for the 1σ distance ranges for these events. For comparison, the green, red, and purple lines show the median sensitivity of CZTI as a function of distance for searches at these three timescales. Note that due to variations in data quality, the limits for individual events may be deeper or shallower than the median values. For comparison, we also show the distance and luminosity of GW170817 reported by B. P. Abbott et al. (2017a, 2017b), though it was not detected by CZTI. The orange histogram at the bottom shows the distribution of median distances to the detected NS events from the R. W. Kiendrebeogo et al. (2023) simulations, which gives us an idea of the relevant range of luminosities that CZTI can probe.
Paper: Bright in the Black: Searching for Electromagnetic Counterparts to Gravitational-wave Candidates in LIGO-Virgo-KAGRA Observation Runs with AstroSat-CZTI
Authors: Gaurav Waratkar, Varun Bhalerao, Dipankar Bhattacharya
Figure caption: Expected fluxes for GW151226 predicted from the three models: neutrino-antineutrino annihilation powered jet mechanism, the Blandford–Znajek mechanism, and a charged black hole model that predict EM radiation from BBH mergers, as discussed in Section 4. The vertical solid lines show our flux upper limits for this event for the three search time bins, the yellow dashed vertical line shows the 1 s 5σ flux sensitivity for the 20–200 keV band of Daksha (V. Bhalerao et al. 2022a), and the blue dashed vertical line marks the 1 s 5σ sensitivity for the 15–350 keV band search with Swift-BAT and Fermi-GBM (C. Fletcher et al. 2023). The three histograms within each panel show the three jet models discussed in Section 4.2.1. For this particular event, our flux upper limits are deep enough to rule out the neutrino wind and charged bh models.
Paper: Bright in the Black: Searching for Electromagnetic Counterparts to Gravitational-wave Candidates in LIGO-Virgo-KAGRA Observation Runs with AstroSat-CZTI
Authors: Gaurav Waratkar, Varun Bhalerao, Dipankar Bhattacharya
Figure caption: Probability of detection of all 57 BBH events as a function of isotropic equivalent luminosity. The black-dashed curve shows the joint detection probability across these 57 BBH events, as described in Section 4.2.2, which shows the detection probability of at least one event out of 57 BBH events. The vertical red line shows the isotropic luminosity of GRB 150914-GBM (V. Connaughton et al. 2016), which is the claimed counterpart to GW150914. Through the nondetections of 57 BBHs, all assumed at the luminosity of GRB 150914-GBM, we can rule out this luminosity of the claimed counterpart with a confidence of 97%.
Paper: The Oscillation in Evolution of Changing-look Blazar OQ 334
Authors: S. S. Ren, R. X. Zhou, Y. G. Zheng, S. J. Kang
Figure caption: The accretion rates ﹩\dot{m}﹩, jet radiation power ﹩\mathrm{log}({P}_{\mathrm{jet}})﹩, photon spectral indices Γ γ , and equivalent widths (EW) for epochs F, B, and T between MJD 54628 and 60387. In the top panel, the red dotted line indicates ﹩\dot{m}=0.1﹩. Purple diamonds and green dots represent the FSRQ (F) and BL Lac (B) epochs. Gray pentagrams and triangles represent the transition epochs (T) from the FSRQ state to the BL Lac state and from the BL Lac state to the FSRQ state, respectively. The gray area represents the 1σ confidence band. It is worth noting that due to the large errors during the T12 epoch, the errors of the T12 epoch are neglected when considering the 1σ confidence band. ﹩\dot{m}﹩ and ﹩\mathrm{log}({P}_{\mathrm{jet}})﹩ of these epochs that are epochs F1, T1, B1, T2, F2, T3, and B2 have been refitted using H 0 = 73.3 km s−1 Mpc−1.
Paper: Bright in the Black: Searching for Electromagnetic Counterparts to Gravitational-wave Candidates in LIGO-Virgo-KAGRA Observation Runs with AstroSat-CZTI
Authors: Gaurav Waratkar, Varun Bhalerao, Dipankar Bhattacharya
Figure caption: Histogram of the flux upper limits calculated for all 61 events as described in Section 2.2 for three search time bins: 0.1 s (blue), 1.0 s (orange), and 10.0 s (green). We also show improvement in our estimation of flux upper limits through the use of the CZTI v2 pipeline (dotted) to CZTI V3 pipeline (solid), as described in Section 2. The median flux upper limit for each time bins are also indicated with a dotted line (V2), and a solid line (V3). As you go from lower time bins to higher, the number of samples in the witness window increases, and hence the cutoff count rate has to increase to achieve the same FAP. As a result, the corresponding flux upper limits are found to reduce with increasing time bins.
Paper: The Oscillation in Evolution of Changing-look Blazar OQ 334
Authors: S. S. Ren, R. X. Zhou, Y. G. Zheng, S. J. Kang
Figure caption: External photon field energy density vs. photon spectral index for epochs F, B, and T during MJD 54628–60387. Green dots and purple prisms correspond to values during the FSRQ (F) and BL Lac (B) epochs, respectively. Gray pentagrams and triangles represent values during the transition epoch (T) from FSRQ to BL Lac and BL Lac to FSRQ, respectively. The light steel blue shading indicates epochs within the range of Γ γ  = 2.0 and Γ γ  = 2.2. The external photon field energy density for different states before the T4 epoch (i.e., MJD 54628–58677) has been refitted according to H 0 = 73.3 km s−1 Mpc−1.