adsabs/AstroCLIMB huggingface dataset:
Paper: High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune
Authors: Samuel H. C. Cabot, Nikku Madhusudhan, Savvas Constantinou, Diana Valencia, Johanna M. Vos, Thomas Masseron, Connor J. Cheverall
Figure caption: The top and bottom panels show 1D slices of S/N near the tentative CH4 signal. The orange curves correspond to the peak in the K  p –V sys plane at K  p  = +30 km s−1 and V sys = −7 km s−1, respectively. For reference, the gray curves correspond to the physical orbital parameters of TOI-732 b, K  p  = +68 km s−1 and V sys = 0 km s−1, respectively (also denoted by vertical dashed lines), indicating the velocity offset of the putative peak signal. As shown in the top panel, we find multiple peaks of comparable strength to our putative signal, albeit at much larger velocity offsets. These additional peaks reduce the statistical confidence of the CH4 signal.
Paper: High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune
Authors: Samuel H. C. Cabot, Nikku Madhusudhan, Savvas Constantinou, Diana Valencia, Johanna M. Vos, Thomas Masseron, Connor J. Cheverall
Figure caption: S/N of the observations. The S/N of the first spectrum in our time series across the IGRINS wavelength range (H band: left; K band: right), obtained at air mass z = 1.08, is shown with the maroon curves in the bottom panel. The S/N exceeds 400 in some parts of the stellar continuum. A fiducial telluric absorption spectrum is shown in the top panel (Hinkle et al. 1995). Some notable features are labeled by their corresponding molecular absorber. The lowest-quality regions in the data primarily correspond to H2O absorption zones, with CO2 and CH4 also having significant contributions. The repetitive arc pattern in the lower panel is due to the blaze function instrumental response of individual spectral orders. For comparison, in the lower panel, we show the S/N of one spectrum used in the study of WASP-77 A b (Line et al. 2021), marked by the dotted orange curve.
Paper: High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune
Authors: Samuel H. C. Cabot, Nikku Madhusudhan, Savvas Constantinou, Diana Valencia, Johanna M. Vos, Thomas Masseron, Connor J. Cheverall
Figure caption: S/N maps for injection/recovery tests for cloudy atmospheric models. These maps are generated in a manner similar to those shown in Figure 3. Model transmission spectra were injected into the data at orbital parameters K  p  = 68 and V sys = 80 km s−1, indicated by the dotted white box. The only molecule considered is CH4, with a varying cloud-top pressure of 10−2, 10−3, 10−4, and 10−5 bar, in the panels proceeding from left to right. Increasing the altitude of the cloud deck, i.e., decreasing the cloud-top pressure, reduces the amplitudes of the spectral features and yields consistently weaker recovered signals.
Paper: High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune
Authors: Samuel H. C. Cabot, Nikku Madhusudhan, Savvas Constantinou, Diana Valencia, Johanna M. Vos, Thomas Masseron, Connor J. Cheverall
Figure caption: Top: S/N map showing a marginal signal for CH4, identical to the corresponding panel in Figure 3. Bottom: same as the top panel, except that out-of-transit frames were used throughout ΔCCF optimization and CCF stacking, instead of in-transit frames. There is no positive enhancement in the resulting S/N map near the expected planet location, lending evidence that the nominal signal is not present in the out-of-transit frames.
Paper: High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune
Authors: Samuel H. C. Cabot, Nikku Madhusudhan, Savvas Constantinou, Diana Valencia, Johanna M. Vos, Thomas Masseron, Connor J. Cheverall
Figure caption: Top: fiducial telluric spectrum, as in Figure 1. Bottom: S/N of first exposure obtained on Night 1 (violet), which was excluded from our analysis. The Night 1 spectra have lower S/N compared to Night 2 (maroon) and do not have adequate out-of-transit frames at low air mass.
Paper: High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune
Authors: Samuel H. C. Cabot, Nikku Madhusudhan, Savvas Constantinou, Diana Valencia, Johanna M. Vos, Thomas Masseron, Connor J. Cheverall
Figure caption: Model transmission spectra used for cross-correlation. Top: transmission spectra with contributions from H2O (blue), CH4 (brown), and NH3 (green), with the spectral baseline set by H2–H2 and H2–He collision-induced absorption. Bottom: cloud-free and cloudy transmission spectra for the CH4 model with a gray-opacity cloud deck placed at various cloud-top pressures. The cloud-free spectrum, shown in brown, is the same in both figures.
Paper: Overmassive Black Holes at Cosmic Noon: Linking the Local and the High-redshift Universe
Authors: Mar Mezcua, Fabio Pacucci, Hyewon Suh, Malgorzata Siudek, Priyamvada Natarajan
Figure caption: One of the 12 “cosmic noon” low-mass galaxies hosting an overmassive BH. Top left: spectral energy distribution fitting of the rest-frame observed ultraviolet, optical, and infrared (when available) photometry (black points) with the best-fit model (black curve), including a combination of the galaxy template (green), an AGN accretion disk component (blue), and an AGN dust torus model (yellow). Top right: PDF for the stellar mass taking into account all possible fractions of AGN emission and providing an upper limit on the stellar mass. So the most probable value (MsPDF blue dashed line) has a higher value than the best-fit stellar mass (MsBEST, red solid line). The 16 and 84 percentile intervals (gray shades) are also indicated. Middle: emission line fitting of the VIPERS spectrum including the continuum emission (in yellow, top panel), and the broad lines (in blue) decomposed into broad (in red) and narrow (in green) components (zoom-in in the bottom panels). Bottom: Subaru Hyper Suprime-Cam image in the i band.
Paper: Overmassive Black Holes at Cosmic Noon: Linking the Local and the High-redshift Universe
Authors: Mar Mezcua, Fabio Pacucci, Hyewon Suh, Malgorzata Siudek, Priyamvada Natarajan
Figure caption:  M BH versus M * for the VIPERS sample of AGN dwarf galaxies at z < 1 of Mezcua et al. (2023; blue squares), the new “cosmic noon” sample of AGN in low-mass galaxies reported here (red squares), and a compilation of JWST AGN in low-mass galaxies at z > 4 (purple squares). We also show for comparison the low-z AGN of Reines & Volonteri (2015; RV2015; blue dots) and the intermediate-z AGN of Suh et al. (2020; Suh+2020; red dots), whose masses have been computed using the same procedure and parameters as the VIPERS samples. The solid black line shows the local + intermediate-z M BH–M * correlation found for the combination of the RV2015 and Suh+2020 samples with a 1σ scatter of 0.5 dex. The red dashed line shows the high-z M BH–M * correlation found by Pacucci et al. (2023) for AGN found at z > 4 by JWST based on the detection of broad Hα or Hβ emission. The green dashed–dotted line shows the Shankar et al. (2016) local correlation for inactive galaxies.
Paper: Overmassive Black Holes at Cosmic Noon: Linking the Local and the High-redshift Universe
Authors: Mar Mezcua, Fabio Pacucci, Hyewon Suh, Malgorzata Siudek, Priyamvada Natarajan
Figure caption: Ratio of M BH/M * vs. redshift for the VIPERS sample of AGN dwarf galaxies at z < 1 of Mezcua et al. (2023), the new VIPERS “cosmic noon” sample of AGN in low-mass galaxies reported here, and a compilation of JWST AGN in low-mass galaxies at z > 4. We show for comparison the nonevolution found by Suh et al. (2020) for z ∼ 0–2.5 (black line, 1σ scatter∼0.5 dex), Sun et al. (2015) for z ∼ 0–2 (brown line), and Setoguchi et al. (2021) for z ∼ 1.2–1.7 (red line), and the z-evolution found by Decarli et al. (2010) for z ∼ 0–3 (dashed blue line), Trakhtenbrot & Netzer (2010) for z ∼ 0.1–2 (dashed yellow line), Bennert et al. (2011) for z ∼ 1–2 (dashed green line, including the data of Merloni et al. 2010), and Pacucci & Loeb (2024) for the JWST z > 4 population of overmassive BHs (dashed purple line). We note that the Suh+2020 sample is the only one for which the BH and stellar masses have been computed using the same procedure and parameters as the VIPERS samples.
Paper: Overmassive Black Holes at Cosmic Noon: Linking the Local and the High-redshift Universe
Authors: Mar Mezcua, Fabio Pacucci, Hyewon Suh, Malgorzata Siudek, Priyamvada Natarajan
Figure caption: Distribution of bolometric luminosity (top) and Eddington ratio (bottom) for the sample of AGN dwarf galaxies at z < 1 of Mezcua et al. (2023), the new “cosmic noon” sample of AGN in low-mass galaxies reported here, and a compilation of JWST AGN in low-mass galaxies at z > 4.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: Spectral energy distributions (SEDs) of the Pop III star tidal flares in the rest frame of the host galaxy. The default parameter set used for plotting this figure and the those subsequent is M BH = 106 M ⊙,  M ⋆ = 300M ⊙ (M 300), Z = 10−5(Z −5), f out = 0.5, f  v  = 1, and β = β  c  = 1.85 (the red solid curve) unless specified otherwise. (a) The evolution of the SEDs at different epochs: t edge/2, t edge (peak luminosity), 2× t edge, and 4× t edge. (b) The SEDs at t = t edge for various Pop III stars of different masses or metallicities and a solar-type star. (c) The dependence of the SEDs (at t = t edge) on M BH. (d) The dependence of the SEDs (at t = t edge) on other parameters including the mass outflow fraction (f out), the ratio between wind velocity and escape velocity (f  v ), and the stellar orbital penetration parameter β (with β  c  = 1.85 being the critical value for full tidal disruption).
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: We show the NIR light curves of Pop III star TDEs in comparison to that of a solar-type star. The integrated NIR flux are in the JWST NIRcam band. All TDEs happen around a MBH with M BH = 106 M ⊙ at z = 10. Color schemes and line styles are the same as in Figure 7. Furthermore, for the default model of Pop III stars (M ⋆ = 300M ⊙ = M 300,  Z = 10−5 = Z −5), we also show the observed NIR light curve when the TDE happens at z = 15 (red thin line) or when the MBH is a UHZ1-like source with M BH = 4 × 107 M ⊙ at z = 10.1 (orange line). The late-time light curves are compared to a power-law decay pattern of t −5/3 (cyan dotted–dashed line). Green and magenta dotted solid lines denote the flux limit of NIRCam (F150W) and WFI (F106), respectively. It is noticed that the observed NIR light curves evolve very slowly due to cosmological time dilation.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: Optical (left) and UV (right) light curves of the Pop III star TDEs around a MBH with M BH = 106 M ⊙ in comparison to that that of a solar-type star. The color and line styles for different stars are the same as in Figure 3. For the fiducial Pop III star TDE model (the red solid curve), we mark the four epochs used in Figure 6(a) (i.e., t edge/2, t edge, 2× t edge, and 4× t edge) using light blue dots. The late-time light curves are fitted with power-law functions that are plotted using cyan dotted–dashed lines. We see that the Pop III star TDEs have much longer rise and decay timescales compared to standard TDEs of normal stars. Furthermore, for a Pop III star TDE, while its optical light curves follow the debris fallback rate relatively closely and peaks around t edge, its UV light curve peaks at a later time and decays much more slowly due to the temperature evolution of the flare.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: The observed fluxes of TDEs of Pop III stars of mass 300M ⊙ (M 300, left panel) and 30M ⊙ (M 30, middle panel) with different metallicities of 10−5 (Z −5, top panel) and 10−9 (Z −9, bottom panel) compared to a solar-type star (right panel) at different epochs (t edge/2, t edge, 2t edge, 4t edge). Green dotted line shows the sensitivity limit of the F150W filter of NIRCam. Magenta dotted line represents the sensitivity limit of the F106 filter of WFI, which has the best sensitivity limit of all the four filters (F106, F129, F158, F184) used in the High Latitude Wide Area Survey. Red shaded regions indicate JWST NIRcam bands. It can be seen that a large part of the fluxes are in the NIR wavelengths and lie above the detection limit of JWST’s NIRCam and Roman’s WFI.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: The dependence of the observed flux at t = t edge on other parameters, such as the MBH mass (M BH), penetration factor (β), mass outflow fraction (f out), and wind velocity (f  v ). Here we stick to the fiducial model of a Pop III star with M ⋆ = 300M ⊙, Z = 10−5. The shaded regions, magenta and green dotted lines are the same as in Figure 8.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: Different forms of IMF for the Pop III stars as listed in Table 1. It should be clarified that Jaacks et al. (2018) calculated Pop III IMF only within the mass range of 1M ⊙–150M ⊙, and Greif et al. (2011) calculated the IMF only within the mass range of 0.1M ⊙–10M ⊙. For this study, we extrapolated all three IMFs to the range of 30M ⊙–300M ⊙.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: The time that the photosphere transits from expansion to recession (t edge) as a function of M BH for various types of stars. The color scheme is the same as Figure 3. t edge is longer for the Pop III stars compared to solar-type stars.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: The Eddington timescale defined as the timescale that the debris mass fallback rate stays above the Eddington accretion rate. It is seen that Pop III star TDEs can stay super-Eddington for very long timescales (up to hundreds of years).
Paper: High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune
Authors: Samuel H. C. Cabot, Nikku Madhusudhan, Savvas Constantinou, Diana Valencia, Johanna M. Vos, Thomas Masseron, Connor J. Cheverall
Figure caption: Recovery of a synthetic signal injected at V sys = 80 and K  p  = 68 km s−1 (denoted by the dotted box), based on our detrending and cross-correlation procedure described in Section 2. The leftmost panel shows the nominal recovery using all frames. In the subsequent panels we have reduced the number of out-of-transit frames, which has the effect of gradually weakening the significance of the recovered signal (from 5.5σ nominally to 3.2σ when only 5 of the available 17 out-of-transit frames are included). For all panels, the color scale is normalized between −5σ and +5σ, and the top panel shows the 1D slice at K  p  = 68 km s−1.
Paper: High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune
Authors: Samuel H. C. Cabot, Nikku Madhusudhan, Savvas Constantinou, Diana Valencia, Johanna M. Vos, Thomas Masseron, Connor J. Cheverall
Figure caption: Results of the bootstrapped cross-correlation analysis. This figure plots the distribution of S/N values at (K  p , V sys) pairs near the tentative CH4 signal, for all 1000 bootstrap trials (where, in each trial, spectra were randomly resampled with replacement at the start of the cross-correlation analysis). The distribution of all S/N values (“All Samples”) is shown by the dotted curve, whereas the filled tan histogram (“Trial Maxima”) shows the distribution of maxima from each trial. The peak S/N of the CH4 signal is marked by a vertical dashed line.
Paper: High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune
Authors: Samuel H. C. Cabot, Nikku Madhusudhan, Savvas Constantinou, Diana Valencia, Johanna M. Vos, Thomas Masseron, Connor J. Cheverall
Figure caption: Air mass as a function of time for Night 1 (violet) and Night 2 (maroon). Exposures during Night 1 took place at significantly higher air mass, which is one of the reasons for the degradation in S/N (Figure 7). Moreover, Night 1 yielded only one post-transit exposure.
Paper: Dark No More: The Low-luminosity Stellar Counterpart of a Dark Cloud in the Virgo Cluster 
Authors: Michael G. Jones, Steven Janowiecki, Swapnaneel Dey, David J. Sand, Paul Bennet, Denija Crnojević, Catherine E. Fielder, Ananthan Karunakaran, Brian R. Kent, Nicolas Mazziotti, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: Left: ALFALFA H I contours overlaid on a griz DECaLS image. BC6 is coincident with a cloud at the NW tip of the H I complex (and is at the same velocity; see Figure 2). The five component clouds of the H I complex are labeled C1–5 as in Kent et al. (2009). The white box (inside cloud C3) indicates the location of BC6 and shows the size of the field of view of the HST image (right panel). The lowest H I column density contour level is 2.2 × 1018 cm−2 (over 20 km s−1), and each subsequent contour is double the previous. The ALFA beam size is shown in the bottom right corner. The white arrows around the edge of the panel indicate the directions toward some of the neighboring galaxies discussed in Section 5.1 and Table 3. Right: HST ACS F814W+F606W color image of BC6. The three components are circled with dashed green ellipses. These are the regions used to produce the CMD of BC6 (Figure 4). The white dotted rectangle indicates the region targeted with HET/LRS2-B.
Paper: Dark No More: The Low-luminosity Stellar Counterpart of a Dark Cloud in the Virgo Cluster 
Authors: Michael G. Jones, Steven Janowiecki, Swapnaneel Dey, David J. Sand, Paul Bennet, Denija Crnojević, Catherine E. Fielder, Ananthan Karunakaran, Brian R. Kent, Nicolas Mazziotti, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: Left: CMD of BC6 within the regions shown in Figure 3 (right). Center: the same CMD with PARSEC isochrones for stellar populations with ages between 10 and 100 Myr. All isochrones have a metallicity of [M/H] = −0.1, roughly matching that measured from emission lines (Table 2), and are scaled to an assumed distance of 16.5 Mpc. Right: CMD of a blank sky region (equal in area to the sum of the apertures in the left panel) of the HST image away from the target. In all panels, the dashed curved line indicates the 90% completeness limit, and the straight dotted line is the 50% limit. All magnitudes are in the Vega system and corrected for Galactic extinction.
Paper: Dark No More: The Low-luminosity Stellar Counterpart of a Dark Cloud in the Virgo Cluster 
Authors: Michael G. Jones, Steven Janowiecki, Swapnaneel Dey, David J. Sand, Paul Bennet, Denija Crnojević, Catherine E. Fielder, Ananthan Karunakaran, Brian R. Kent, Nicolas Mazziotti, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: Left: NGVS ugi image of BC6, similar to the image in which it was originally identified. Right: GALEX NUV+FUV image similar to that used for the original identification and covering the same field as in the left panel. The source is deliberately unlabeled, but its components are circled in Figure 3 (right), which shows a similar field of view. Without the comparison of the optical and UV images, blue blobs would be almost impossible to identify. The bright blue speckles in the top left of the right panel are an artifact from the GALEX FUV data.
Paper: Dark No More: The Low-luminosity Stellar Counterpart of a Dark Cloud in the Virgo Cluster 
Authors: Michael G. Jones, Steven Janowiecki, Swapnaneel Dey, David J. Sand, Paul Bennet, Denija Crnojević, Catherine E. Fielder, Ananthan Karunakaran, Brian R. Kent, Nicolas Mazziotti, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: GBT H I spectrum at the location of BC6. The vertical dashed line indicates the velocity of BC6 determined from Hα line emission (Section 3.5). The profile is double horned because the large GBT beam includes some emission from the adjacent H I cloud just to the SE (denoted as C4 by Kent et al. 2009), which is at a slightly higher velocity.
Paper: Dark No More: The Low-luminosity Stellar Counterpart of a Dark Cloud in the Virgo Cluster 
Authors: Michael G. Jones, Steven Janowiecki, Swapnaneel Dey, David J. Sand, Paul Bennet, Denija Crnojević, Catherine E. Fielder, Ananthan Karunakaran, Brian R. Kent, Nicolas Mazziotti, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: HET LRS2-B spectrum of BC6 showing the Hα, Hβ, [N II], and [O III] lines. The marked wavelengths of each line (vertical dashed lines) are all shifted to match the redshift of Hα. The vertical dotted lines indicate ±2 standard deviations of the Gaussian fit to the Hα line. This is also the window that was used to extract the line fluxes of all other lines (Table 2).
Paper: The Influence of Thermonuclear Bursts on Polar Caps of the Accreting X-Ray Millisecond Pulsar MAXI J1816-195
Authors: Long Ji, Mingyu Ge, Yupeng Chen, Zhaosheng Li, Peng-Ju Wang, Shu Zhang, Shuang-Nan Zhang
Figure caption: Averaged pulse profiles during thermonuclear bursts in 8–30 keV (upper) and 30–100 keV (lower), where dashed lines are best-fitting models assuming a sinusoidal shape. The burst and nonburst pulse profiles correspond to the left and right vertical axes, respectively. We set the same scale for both axes but with different median values.
Paper: The Influence of Thermonuclear Bursts on Polar Caps of the Accreting X-Ray Millisecond Pulsar MAXI J1816-195
Authors: Long Ji, Mingyu Ge, Yupeng Chen, Zhaosheng Li, Peng-Ju Wang, Shu Zhang, Shuang-Nan Zhang
Figure caption: Parameters describing pulse profiles using a sinusoidal model. The red dashed line represents the time zero corresponding to the averaged burst peak.
Paper: The Influence of Thermonuclear Bursts on Polar Caps of the Accreting X-Ray Millisecond Pulsar MAXI J1816-195
Authors: Long Ji, Mingyu Ge, Yupeng Chen, Zhaosheng Li, Peng-Ju Wang, Shu Zhang, Shuang-Nan Zhang
Figure caption: Averaged lightcurves of thermonuclear bursts in MAXI J1816-195 observed with Insight-HXMT/ME (upper) and HE (bottom) detectors. The shaded region represents the burst interval.
Paper: The Influence of Thermonuclear Bursts on Polar Caps of the Accreting X-Ray Millisecond Pulsar MAXI J1816-195
Authors: Long Ji, Mingyu Ge, Yupeng Chen, Zhaosheng Li, Peng-Ju Wang, Shu Zhang, Shuang-Nan Zhang
Figure caption: Averaged background-subtracted lightcurves of 12 thermonuclear bursts observed in the low-background regions of Insight-HXMT/HE. The shaded region represents the burst interval.
Paper: The Influence of Thermonuclear Bursts on Polar Caps of the Accreting X-Ray Millisecond Pulsar MAXI J1816-195
Authors: Long Ji, Mingyu Ge, Yupeng Chen, Zhaosheng Li, Peng-Ju Wang, Shu Zhang, Shuang-Nan Zhang
Figure caption: A representative example of averaged simulated lightcurves. This suggests the long-term variability of the HE background can not be fully eliminated by stacking lightcurves.