adsabs/AstroCLIMB huggingface dataset:
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: Quasar space densities at z ∼ 6. The red circles represent our results from the total survey area, while the red hexagons are from the three individual fields where high-redshift quasars are identified. The other symbols represent those in the literature (Willott et al. 2010; Jiang et al. 2016; Onoue et al. 2017; Matsuoka et al. 2018c; Parsa et al. 2018; Giallongo et al. 2019; Grazian et al. 2020). The filled (open) symbols are from the surveys based on rest-UV photometry (X-ray detection). The blue line shows the parametric LF of quasar (Matsuoka et al. 2018c). The black solid (dashed) line represents the quasar LF model with (without) the outshining effect (Kim & Im 2021). The parametric LF of UV dropout objects (or AGN+galaxy; Harikane et al. 2021) is auxiliary, shown as the gray crosses with dotted line.
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: Selection completeness in each field as a function of z and M 1450, F field(z, M 1450), divided into the cases of ﹩{i}_{1}^{{\prime} }﹩ (top row) and ﹩{i}_{2}^{{\prime} }﹩ (bottom row) bands. The color bar shows the completeness level. The orange circles are the spec-identified quasars, listed in Table 3. The red boxes indicate the two bins for estimating space density.
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: Total selection completeness as a function of z and M 1450. The symbols are the same as in Figure 10. The red boxes indicate the two bins for estimating space density.
Paper: Searching the SETI Ellipsoid with Gaia
Authors: James R. A. Davenport, Bárbara Cabrales, Sofia Sheikh, Steve Croft, Andrew P. V. Siemion, Daniel Giles, Ann Marie Cody
Figure caption: Schematic diagram of the SETI Ellipsoid framework. A civilization (black dot) could synchronize a technosignature beacon with a noteworthy source event (green dot). The arrival time of these coordinated signals is defined by the time-evolving ellipsoid, whose foci are Earth and the source event. Stars outside the Ellipsoid (blue dot) may have transmitted signals in coordination with their observation of the source event, but those signals have not reached Earth yet. For stars far inside the Ellipsoid (pink dot), we have missed the opportunity to receive such coordinated signals.
Paper: Searching the SETI Ellipsoid with Gaia
Authors: James R. A. Davenport, Bárbara Cabrales, Sofia Sheikh, Steve Croft, Andrew P. V. Siemion, Daniel Giles, Ann Marie Cody
Figure caption: Galactocentric Y,Z location for stars in the GCNS, with points colored by their designation within the SETI Ellipsoid framework for SN 1987A. 192,489 stars have seen SN 1987A but we could not yet have received a synchronized transmission (blue points). 138,823 stars have not observed SN 1987A (red points). There are 25,817 stars inside the current SETI Ellipsoid for SN 1987A (purple points). At time of writing (mid 2022), 134 stars from the GCNS are within 0.1 lyr of the SN 1987A Ellipsoid surface. The location of the Sun is also indicated (yellow cross).
Paper: Searching the SETI Ellipsoid with Gaia
Authors: James R. A. Davenport, Bárbara Cabrales, Sofia Sheikh, Steve Croft, Andrew P. V. Siemion, Daniel Giles, Ann Marie Cody
Figure caption: Two dimensional histogram of the symmetrized distance errors for 331k stars in the GCNS, with the median (dashed line) and mode (solid line) distance errors shown. Typical uncertainties are less than 1 lyr for all stars within the 100 pc sample the GCNS, making this sample amenable for use in searching for synchronized signals via the SETI Ellipsoid framework.
Paper: Searching the SETI Ellipsoid with Gaia
Authors: James R. A. Davenport, Bárbara Cabrales, Sofia Sheikh, Steve Croft, Andrew P. V. Siemion, Daniel Giles, Ann Marie Cody
Figure caption: To-scale drawing of the information front (green dashed line) and the SETI Ellipsoid (black solid line) for SN 1987A, in an arbitrary coordinate frame oriented along the line of sight to the Large Magellanic Cloud. Though SN 1987A was observed more than 35 yr ago, very few synchronized signals could have reached us thus far.
Paper: Searching the SETI Ellipsoid with Gaia
Authors: James R. A. Davenport, Bárbara Cabrales, Sofia Sheikh, Steve Croft, Andrew P. V. Siemion, Daniel Giles, Ann Marie Cody
Figure caption: Earth-centered galactocentric Y,Z positions for a slice of 47,484 stars within the GCNS with ∣X∣ < 10 pc. Points are colored by the date when each star star intersects the SN 1987A SETI Ellipsoid. Contours show the progression of the SETI Ellipsoid each century.
Paper: The Rapid Rotation of the Strongly Magnetic Ultramassive White Dwarf EGGR 156
Authors: Kurtis A. Williams, J. J. Hermes, Zachary P. Vanderbosch
Figure caption: Periodograms for EGGR 156 (left panels) and the spectral window function for the fundamental frequency (right panels) scaled to the fit amplitude. Shown are the periodograms for Series 2 (top panel) and the entire combined BG40 data set (middle panel). Horizontal long-dashed, magenta lines show the adopted ﹩4\left\langle \,{\rm{A}}\,\right\rangle ﹩ significance threshold. The bottom panel shows the entire data set after prewhitening by the fundamental frequency f 0 and the harmonic 2f 0; no residual significant peaks remain. Vertical dotted lines indicate the location of harmonics f 0, 2f 0, and 3f 0.
Paper: The Rapid Rotation of the Strongly Magnetic Ultramassive White Dwarf EGGR 156
Authors: Kurtis A. Williams, J. J. Hermes, Zachary P. Vanderbosch
Figure caption: Left: all BG40 data folded at best-fitting frequency (top) and binned into 30 phase bins (bottom). The solid line in the top plot is the best-fitting sinusoid. Error bars on the bottom panel indicate the uncertainty in the mean for that bin. Right: points with error bars are phase folded and binned light curves for g (top), r (middle), and i (bottom) observations compared to the BG40 binned light curve (histogram). The gri data were binned into 20 bins; again the error bars show the uncertainty in the mean for the bin. The folded light curves in r and i show qualitative evidence of phase lag.
Paper: The Rapid Rotation of the Strongly Magnetic Ultramassive White Dwarf EGGR 156
Authors: Kurtis A. Williams, J. J. Hermes, Zachary P. Vanderbosch
Figure caption: Periodograms for the g (top panel), r (second panel), and i (third panel) observations of EGGR 156. The bottom panel shows the spectral window for the frequency f 0 scaled to the g-band fit amplitude. No significant i-band signal is observed, although the noise is significantly higher in that band. The vertical dashed line indicates the best frequency as determined from BG40 observations.
Paper: The Rapid Rotation of the Strongly Magnetic Ultramassive White Dwarf EGGR 156
Authors: Kurtis A. Williams, J. J. Hermes, Zachary P. Vanderbosch
Figure caption: Light curves for all time-series observations of EGGR 156. Left: all BG40 time-series observations. Right: the interleaved gri observations. In all panels, the horizontal axes give the time in hours from the start of each series (see Table 1). The vertical axes show the fractional change in flux compared to the mean flux for that filter. The modulation can be seen by visual inspection in the BG40 band (left panels) and the g band (top right panel), but is barely visible in r (middle right panel) and not at all in i (bottom right panel).
Paper: Coronal and Chromospheric Emission in A-type Stars
Authors: Hans Moritz Günther, Carl Melis, J. Robrade, P. C. Schneider, Scott J. Wolk, Rakesh K. Yadav
Figure caption: Comparison of the X-ray luminosity in A-type stars with data for earlier and later spectral types. Early A-type stars are fainter in X-rays than other spectral types. Note that the ROSAT catalog compiled by Freund (2022) does not resolve most binaries and thus especially the data points listed in the range T eff = 7500–10000 K represent the L bol from an A-star primary and the L  X  from an unresolved late-type companion. This highlights the importance of carefully selecting a sample of single A stars as done in this work (black points).
Paper: Coronal and Chromospheric Emission in A-type Stars
Authors: Hans Moritz Günther, Carl Melis, J. Robrade, P. C. Schneider, Scott J. Wolk, Rakesh K. Yadav
Figure caption: X-ray and C III 977 Å line flux. Both fluxes are shown relative to the star’s bolometric luminosity. Stars cooler than about 8000 K are all detected in X-rays and C III 977 Å, while stars that are significantly hotter are at least an order of magnitude fainter. The solar data is taken from (Ayres 1997), the other UV fluxes from Simon et al. (2002).
Paper: Coronal and Chromospheric Emission in A-type Stars
Authors: Hans Moritz Günther, Carl Melis, J. Robrade, P. C. Schneider, Scott J. Wolk, Rakesh K. Yadav
Figure caption: Observations with the Chandra/HRC. The blue circles mark a 1″ radius around the expected position of the target accounting for proper motion at the time of the observation. For τ 3 Eri, the dotted circle accounts for the coordinate offset discussed in the text.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: The TSM used by the TESS Atmospheric Characterization Working Group to classify the suitability of atmospheres for characterization (Kempton et al. 2018) for TPCs that are potential targets for Ariel’s tier 1 and 2 surveys. In tier 1, Ariel will be capable of observing planets with far lower TSMs than the statistical sample considered in Kempton et al. (2018; TSM > 90), with some planets that have TSM ∼ 40 still being considered suitable for the mission. We note that the metric was designed only for JWST NIRISS and, therefore, is not a robust method for assessing the suitability for study with Ariel.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Known (left) and TPC (right) systems that host at least two worlds that could be studied in tier 1 with Ariel. Colors indicate the suitability of characterization (white: not suitable; light blue: tier 1; dark blue: tier 2), while the size of the circles reflects the planet’s radius. Those below the dotted line were listed as having been discovered by TESS in the NASA Exoplanet Archive.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Relationship between the number of tier 1 and 2 planets that can be observed during the prime mission life. The red region is forbidden; by their very definition, one cannot observe more targets in tier 2 than in tier 1. We also show what could be achieved with a 2 yr mission extension. In all cases, 50 planets are assumed to be studied in tier 3, and 10% of Ariel’s science time is left for tier 4 observations and complementary science programs.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Constraints on the main carbon- and oxygen-bearing species from our retrievals for TOI-1130 b (red) and c (blue). The solid lines show the best-fit model, while the 1σ uncertainties are highlighted by the shaded regions. The input values are given by the dotted lines. While the H2O and CO abundances are well constrained, the CO2 profile is less so, as is CH4 in the upper atmosphere. Increasing the number of observations might improve our knowledge of these molecules and thus elemental ratios such as C/O. Ariel probes from the cloud deck at 1e3 Pa up to roughly 1e1.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Temperature and radius distribution of known planets, including those found by TESS (left), and these known planets in addition to the current TPCs (right) for worlds with radii smaller than 3 R ⊕ that are suitable for tier 1 study with Ariel.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Sky locations of the example MRS, indicated by stars, with the brightest 35 million stars from the Gaia database (Gaia Collaboration et al. 2016, 2018) plotted in the background. The host stars are spread across the sky but with a lower density in the galactic plane. Transit searches here are harder due to the dilution of sources, but this will also be true of Ariel observations; thus, targets in this plane may be less advantageous anyway.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Example MRS derived from currently known planets and the TPCs. The observing campaign shown would require 21,944 hr of telescope time, equivalent to 88.5% of Ariel’s available science time in the prime mission life (∼24,800 hr). We note that around 10% of the time is expected to be left for tier 4 observations and complementary science.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Posterior distributions for our retrievals of TOI-1130 b and c. For the assumed atmospheric metallicities and C/O ratios, Ariel would be able to distinguish between them and thus uncover a mass–metallicity trend in the system, as well as inferring differences in their formation.
Paper: Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Distribution of Galactic velocity dispersion for Monte Carlo samples of hosts of aligned and misaligned hot Jupiters. At each iteration, the sky-projected stellar obliquity is sampled from within its uncertainty. Systems with ∣λ∣ < 12°.8 are considered aligned. The solid vertical lines indicate the median Galactic velocity dispersion of the samples, the dashed vertical lines indicate the 16th and 84th percentiles, and the dashed–dotted vertical lines indicate the 2.5th and 97.5th percentiles. Top: systems for which the fractional convective envelope mass of the host star is less than the median value within the sample, and the alignment timescale should be long in the Albrecht et al. (2012) model. Across Monte Carlo realizations of λ within its uncertainty, typical sample sizes for the misaligned and aligned systems are ﹩{31}_{-1}^{+2}﹩ and ﹩{20}_{-2}^{+1}﹩, respectively. We find that aligned systems have a smaller velocity dispersion than misaligned systems at roughly 3.6σ, contrary to what would be expected if tides are damping misalignments over time. Bottom: systems for which the host star has a fractional convective envelope mass larger-than-the-median value within the sample, and the alignment timescale should be short. Typical sample sizes for the misaligned and aligned systems are ﹩{20}_{-3}^{+2}﹩ and ﹩{31}_{-2}^{+3}﹩, respectively. Aligned systems have a smaller velocity dispersion than misaligned systems at roughly 1.2σ.
Paper: Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Sky-projected stellar obliquities of transiting hot Jupiter host stars plotted against stellar mass, stellar age, a/R *, planet-to-star mass ratio, and convective envelope mass as a fraction of stellar mass. Blue points indicate systems for which our modeling of the host star determines it has a surface convective envelope. Red points indicate systems for which the host star has no mass in a surface convective envelope. According to tidal theory, systems with small scaled semimajor axes and larger planet-to-star mass ratios should align more quickly. According to the Albrecht et al. (2012) model for realignment, systems with more mass in the host star’s convective envelope should align more quickly. Top: stellar mass, M *. M * alone is not a perfect proxy for the convective envelope mass, motivating our use of stellar models. Top-middle: stellar age, t *. Older systems appear to more often have low stellar obliquities, but stellar mass confounds any apparent relationship. Middle: scaled semimajor axis a/R *. Misalignments persist even at small values of a/R * in contrast to the strong a/R * dependence of tides. Bottom middle: mass ratio M p/M *. Higher mass-ratio systems appear to be more well aligned. Bottom left: distribution of stellar obliquities for systems in which the host star has no convective envelope. Bottom middle: fraction of stellar mass in the convective envelope, M CE/M *. High obliquities are present regardless of the presence of the convective envelope. Bottom right: distribution of stellar obliquities for systems in which the host stars have mass in their convective envelopes.
Paper: Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Comparison between the photospheric stellar parameters derived from high-resolution spectroscopy and isochrone analysis. Solid gray lines indicate the line y = x. Top left: comparison between the stellar effective temperature predictions. Dashed gray lines indicate 200 K above and below the one-to-one correspondence. The parameters output by the two methods display good agreement. Top right: comparison between the predicted surface gravities. The isochronal surface gravities are consistent with the surface gravities expected for main-sequence stars. Dashed gray lines indicate 0.1 dex above and below one-to-one correspondence. Bottom left: comparison between the metallicity estimates. Dashed gray lines indicate 0.1 dex above and below one-to-one correspondence. While in many cases the isochronal metallicity is higher, this is not unexpected as hot Jupiter host stars are preferentially metal-rich. Bottom right: comparison between the extinction predictions of the 3D dust maps and those of isochrones. Most stars have low extinction, consistent with their small distances.
Paper: Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Difference in Galactic velocity dispersion between samples of hot Jupiter hosts and matched field stars. The sample size is matched to that of the number of aligned systems hosted by stars with smaller-than-median fractional convective envelope masses. The black line indicates the difference between the median Galactic velocity dispersions of the misaligned and aligned system populations hosted by stars with smaller-than-median fractional convective envelope masses. Less than 1% of the hot Jupiter host-star samples and matched control samples exhibit a Galactic velocity dispersion offset larger than those of the misaligned and aligned systems hosted by stars with smaller-than-median fractional convective envelope masses. Therefore, we argue that it is likely that the misaligned population genuinely has a larger Galactic velocity dispersion than the aligned population hosted by stars with smaller-than-median fractional convective envelope masses, implying a larger relative age for the misaligned population.
Paper: Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Stellar obliquities of hot Jupiter host stars plotted against the host stars’ isochronal ages scaled to their main-sequence lifetimes. The main-sequence lifetimes of the stars in the sample are determined using terminal-age main sequence of the MIST evolutionary tracks for a star of that mass and metallicity. Stars with larger-than-median fractional convective envelope masses are shown as blue points, and stars with smaller-than-median fractional convective envelope masses are shown as orange points. Misalignments are present even for stars that have lived out a significant portion of their main-sequence lifetimes. Hence, it is unlikely that tidal realignment is a significantly faster process than tidal orbital decay.
Paper: Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Fraction of stellar mass in the surface convective envelope as a function of T eff. Point color indicates the ﹩\mathrm{log}g﹩ predicted by isochrones. The output of the MESA models reproduces the expected general trend of increasing mass in the convective envelope at lower T eff, with slightly evolved stars having more mass in their convective envelopes.
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Left: the TESS light curve shows a strong rotational modulation. The Lomb–Scargle periodogram of the year 1 TESS light curves is shown in pink, the periodogram for the extended mission is shown in teal, and the periodogram for the combined TESS light curves is shown in navy. Each season of the WASP observations is shown in gray. The rotation period of ∼12.5 days is consistently measured in the 17 sectors observed by TESS and the five seasons observed by WASP. Right: normalized TESS light curve detrended using the methods described in Vanderburg et al. (2019), phase folded over the measured stellar rotation period extracted from the combined primary and extended TESS observations. The phased points are colored based on the time of observation, showing that while the phase curve morphology changes slightly over time, the measured period is consistent with data from both year 1 (blue tint) and year 3 (pink tint).