adsabs/AstroCLIMB huggingface dataset:
Paper: Anomalous Flux in the Cosmic Optical Background Detected with New Horizons Observations
Authors: Tod R. Lauer, Marc Postman, John R. Spencer, Harold A. Weaver, S. Alan Stern, G. Randall Gladstone, Richard P. Binzel, Daniel T. Britt, Marc W. Buie, Bonnie J. Buratti, Andrew F. Cheng, W. M. Grundy, Mihaly Horányi, J. J. Kavelaars, Ivan R. Linscott, Carey M. Lisse, William B. McKinnon, Ralph L. McNutt, Jeffrey M. Moore, J. I. Núñez, Catherine B. Olkin, Joel W. Parker, Simon B. Porter, Dennis C. Reuter, Stuart J. Robbins, Paul M. Schenk, Mark R. Showalter, Kelsi N. Singer, Anne. J. Verbiscer, and Leslie A. Young
Figure caption: The present result is compared to previous COB measures over the wavelengths spanned by the LORRI passband. Our NH21 COB flux (for the Zemcov DGL) is shown in gray, offset to the blue for clarity. Direct COB flux measurements are shown as points with error bars. The Zemcov et al. (2017) flux limit and the Mattila et al. (2017) 0.52 μm limit are shown as 2σ upper limits with 1σ arrows. IGL estimates are shown as lines with 1σ bounds. COB fluxes inferred from VHE γ-rays are shown as shaded bands.
Paper: The First Near-infrared Transmission Spectrum of HIP 41378 f, A Low-mass Temperate Jovian World in a Multiplanet System
Authors: Munazza K. Alam, James Kirk, Courtney D. Dressing, Mercedes López-Morales, Kazumasa Ohno, Peter Gao, Babatunde Akinsanmi, Alexandre Santerne, Salomé Grouffal, Vardan Adibekyan, Susana C. C. Barros, Lars A. Buchhave, Ian J. M. Crossfield, Fei Dai, Magali Deleuil, Steven Giacalone, Jorge Lillo-Box, Mark Marley, Andrew W. Mayo, Annelies Mortier, Nuno C. Santos, Sérgio G. Sousa, Emma V. Turtelboom, Peter J. Wheatley, and Andrew M. Vanderburg
Figure caption: Top: example HIP 41378 f stellar spectrum for the HST/WFC3 G141 grism. The vertical bands denote the 0.018 μm wavelength channels adopted for the spectroscopic light curves. Middle: raw (top) and detrended (bottom) white light curve, excluding the first orbit and the first exposure of each subsequent orbit (points). The raw light curve has been shifted vertically by an arbitrary constant for clarity. Overplotted is the best-fitting analytic light-curve model (line). Epochs most affected by South Atlantic Anomaly passages are denoted by the gray shading. Bottom: rms residuals of the transit fit in ppm (left; points) and 1σ range of the residuals (dotted lines), as well as the distribution of residuals (right).
Paper: The First Near-infrared Transmission Spectrum of HIP 41378 f, A Low-mass Temperate Jovian World in a Multiplanet System
Authors: Munazza K. Alam, James Kirk, Courtney D. Dressing, Mercedes López-Morales, Kazumasa Ohno, Peter Gao, Babatunde Akinsanmi, Alexandre Santerne, Salomé Grouffal, Vardan Adibekyan, Susana C. C. Barros, Lars A. Buchhave, Ian J. M. Crossfield, Fei Dai, Magali Deleuil, Steven Giacalone, Jorge Lillo-Box, Mark Marley, Andrew W. Mayo, Annelies Mortier, Nuno C. Santos, Sérgio G. Sousa, Emma V. Turtelboom, Peter J. Wheatley, and Andrew M. Vanderburg
Figure caption: Broadband transmission spectrum for HIP 41378 f (black points), compared to 1D radiative-convective forward models (colored lines) for a clear atmosphere with metallicities 1×, 30×, and 300× solar, example hazy and ringed models, as well as a flat line (gray atmosphere). Top: the WFC3 transmission spectrum and the measured optical transit depth measurement from K2 (gray diamond; Santerne et al. 2019). Middle: zoom-in to the WFC3 data presented in this work. Bottom: zoom-out to the full spectrum, including mid-infrared wavelengths accessible with JWST.
Paper: The First Near-infrared Transmission Spectrum of HIP 41378 f, A Low-mass Temperate Jovian World in a Multiplanet System
Authors: Munazza K. Alam, James Kirk, Courtney D. Dressing, Mercedes López-Morales, Kazumasa Ohno, Peter Gao, Babatunde Akinsanmi, Alexandre Santerne, Salomé Grouffal, Vardan Adibekyan, Susana C. C. Barros, Lars A. Buchhave, Ian J. M. Crossfield, Fei Dai, Magali Deleuil, Steven Giacalone, Jorge Lillo-Box, Mark Marley, Andrew W. Mayo, Annelies Mortier, Nuno C. Santos, Sérgio G. Sousa, Emma V. Turtelboom, Peter J. Wheatley, and Andrew M. Vanderburg
Figure caption: Equilibrium temperature vs. the 1.4 μm H2O feature amplitude (AH) for the cooler (Teq < 1000 K) planets sample from Dymont et al. (2021) (points) and HIP 41378 f (orange star). There is no clear trend in AH with planetary temperature.
Paper: The First Near-infrared Transmission Spectrum of HIP 41378 f, A Low-mass Temperate Jovian World in a Multiplanet System
Authors: Munazza K. Alam, James Kirk, Courtney D. Dressing, Mercedes López-Morales, Kazumasa Ohno, Peter Gao, Babatunde Akinsanmi, Alexandre Santerne, Salomé Grouffal, Vardan Adibekyan, Susana C. C. Barros, Lars A. Buchhave, Ian J. M. Crossfield, Fei Dai, Magali Deleuil, Steven Giacalone, Jorge Lillo-Box, Mark Marley, Andrew W. Mayo, Annelies Mortier, Nuno C. Santos, Sérgio G. Sousa, Emma V. Turtelboom, Peter J. Wheatley, and Andrew M. Vanderburg
Figure caption: Transit times vs. transit epoch for HIP 41378 f for observed transits from previous K2 and NGTS analyses (Vanderburg et al. 2016; Becker et al. 2019; Bryant et al. 2021) compared to the current HST analysis (open black circles). We compare the transit times predicted by Bryant et al. (2021) (green circles) with our new transit predictions based on the HST transit midpoint (open blue circles). The dashed black line marks the linear ephemeris calculated using the period and transit midpoint from Santerne et al. (2019), along with the median TTV signal (orange line) and 1σ uncertainty (shaded region).
Paper: Tidal Dissipation Due to Inertial Waves Can Explain the Circularization Periods of Solar-type Binaries
Authors: Adrian J. Barker
Figure caption: Top: tidal quality factor ﹩\langle {Q}_{\mathrm{IW}}^{{\prime} }\rangle ﹩ multiplied by ﹩{\epsilon }_{{\rm{\Omega }}}^{2}﹩ as a function of age, due to (frequency-averaged) dissipation of inertial waves in the convective envelopes of various stars with the masses (in solar masses) indicated in the legend. Bottom: same, except that Prot = 10 days following the evolution of each star. The most efficient dissipation is found during both the PMS and as the star evolves off the MS.
Paper: Tidal Dissipation Due to Inertial Waves Can Explain the Circularization Periods of Solar-type Binaries
Authors: Adrian J. Barker
Figure caption: Evolution of the stellar radius R (normalized by the solar radius R⊙) with age (t) for the stars in our mass range. The radius is largest during the PMS (t ≲ 107 yr) and in later phases as the stars evolve off the MS (t ≳ O(109) yr).
Paper: Tidal Dissipation Due to Inertial Waves Can Explain the Circularization Periods of Solar-type Binaries
Authors: Adrian J. Barker
Figure caption: Pcirc as a function of age (assuming Prot = Porb), due to the dissipation of inertial waves (top), internal gravity waves (middle), and equilibrium tides (bottom; where νE is equal to the high-frequency portion of νFIT in solid and νE = uclc/3 in dashed lines—note: the latter is unphysical), computed for a range of stellar masses (legend, in solar masses). We overplot the observations compiled by Nine et al. (2020) as black symbols with labels. Inertial wave dissipation can explain the observed binary circularization periods.
Paper: Tidal Dissipation Due to Inertial Waves Can Explain the Circularization Periods of Solar-type Binaries
Authors: Adrian J. Barker
Figure caption: Synchronization period Psync, assuming an initial rotation period Prot = 5 days. Because Psync(t) > Pcirc(t) due to inertial waves, this indicates that spin–orbit synchronization is a reasonable assumption for the purposes of Figure 3.
Paper: Tidal Dissipation Due to Inertial Waves Can Explain the Circularization Periods of Solar-type Binaries
Authors: Adrian J. Barker
Figure caption: Top: Prot as a function of age for a solar-mass star with three initial rotation periods computed with star-disk locking and magnetic braking but ignoring tides. Bottom: Pcirc from solving Equation (2) for inertial wave dissipation using the above Prot as a function of age. This can be compared with Figure 3 and indicates that PMS circularization is efficient without assuming Porb = Prot.
Paper: Possible TeV Gamma-Ray Binary Origin of HESS J1828–099
Authors: Agnibha De Sarkar, Nirupam Roy, Pratik Majumdar, Nayantara Gupta, Andreas Brunthaler, Karl M. Menten, Sergio A. Dzib, Sac Nicté X. Medina, and Friedrich Wyrowski
Figure caption: (a) Data and model spectrum fit, the residual, and the ratio (data/model) for the best-fit values given in the upper panel of Table 1. The model used in this case is constant∗tbabs∗(cutoffpl∗gabs + Gauss). FPMA and FPMB data points and best fits are shown in black and red, respectively. (b) Data and model spectrum fit, the residual, and the ratio (data/model), after addition of a power-law component with the best-fit model used in (a). Model used in this case is constant∗tbabs∗(cutoffpl∗gabs + Gauss + pow). The color scheme is the same as in (a).
Paper: Possible TeV Gamma-Ray Binary Origin of HESS J1828–099
Authors: Agnibha De Sarkar, Nirupam Roy, Pratik Majumdar, Nayantara Gupta, Andreas Brunthaler, Karl M. Menten, Sergio A. Dzib, Sac Nicté X. Medina, and Friedrich Wyrowski
Figure caption: (a) H.E.S.S. significance map centered on HESS J1828–099. The color bar denotes the ﹩\sqrt{\mathrm{TS}}﹩ value of the region. The gray circle represents the extent to which a 1D Gaussian template was fitted, and the white circle signifies the region within which spectral points for HESS J1828–099 were extracted. Morphologies of 4FGL J1830.2–1005 at different energy ranges are shown with the green dotted line (0.3–1 GeV) and the cyan dashed line (1–500 GeV). Blue dotted–dashed line signifies a spatial extension of the 4FGL in the entire considered energy range (0.3–500 GeV). The RXTE position of pulsar XTE J1829–098 (Halpern & Gotthelf 2007), along with the 99% confidence region (Markwardt et al. 2004), is also shown in yellow. The Chandra position of the pulsar is shown with a light-blue star. (b) Variation of the delta log-likelihood value of 4FGL J1830.2–1005 modeled with radial disks of different radii. The blue shaded region indicates the uncertainty estimate of the best-fit extension of 4FGL J1830.2–1005. (c) The combined THOR and VGPS 1.4 GHz image and (d) the GLOSTAR 5.8 GHz image showing the radio continuum emission from the field containing HESS J1828–099, 4FGL J1830.2–1005, and the pulsar XTE J1829–098. The Chandra position of the pulsar is marked with a star, and the RXTE error region is shown with a black ellipse. Spatial extent marked for the H.E.S.S. and the 4FGL sources (0.3–500 GeV) is the same as in (a). Plausible radio counterpart of the binary system is marked by a white circle.
Paper: Possible TeV Gamma-Ray Binary Origin of HESS J1828–099
Authors: Agnibha De Sarkar, Nirupam Roy, Pratik Majumdar, Nayantara Gupta, Andreas Brunthaler, Karl M. Menten, Sergio A. Dzib, Sac Nicté X. Medina, and Friedrich Wyrowski
Figure caption: Multiwavelength SED of the source HESS J1828–099 and corresponding IC dominated (a) model 1 and (b) model 2, obtained using GAMERA. The unabsorbed power-law X-ray SED obtained from NuSTAR data analysis in the outburst phase of XTE J1829–098 is shown with gray data points. The same unabsorbed X-ray SED, time-averaged over the orbital period of XTE J1829–098 (Halpern & Gotthelf 2007) is shown with teal data points. The H.E.S.S. data, shown in blue, were taken from Abdalla et al. (2018a). We have analyzed the Fermi-LAT data and the corresponding SED from 4FGL J1830.2–1005 is shown in red. The 3σ upper limits at radio range, obtained at the Chandra position of XTE J1829–098, observed by THOR (black), GLOSTAR (maroon), and TGSS (green), are shown in (a) with downward arrows. In (b), flux values of the putative radio source from these surveys are shown with the same color scheme. In (c) and (d), we present the cooling timescale and energy-loss rate of model 1, at time t = tage ≈107 yr. In (e) and (f), we plot the same as (c) and (d), for model 2.
Paper: Possible TeV Gamma-Ray Binary Origin of HESS J1828–099
Authors: Agnibha De Sarkar, Nirupam Roy, Pratik Majumdar, Nayantara Gupta, Andreas Brunthaler, Karl M. Menten, Sergio A. Dzib, Sac Nicté X. Medina, and Friedrich Wyrowski
Figure caption: Results of 1000 Monte Carlo simulations to test the significance of the subdominant power-law component depicting shock. The blue solid histogram shows the frequency (y-axis) of Δχ2 values (x-axis) obtained in the simulations. The red dashed line shows the observed ﹩{\rm{\Delta }}{\chi }_{\mathrm{obs}}^{2}﹩ = 9.04.
Paper: Gradual Sequestration of Water at Lunar Polar Conditions due to Temperature Cycles
Authors: Norbert Schorghofer
Figure caption: Schematic illustration of three types of water ice storage in lunar soil. (a) Cold traps lie within permanent shadow (gray) and are so cold that sublimation into vacuum is less than the amount that was delivered to the cold trap over time. (b) Adsorbed water molecules migrate into the porous subsurface until they reach depths beyond the influence of diurnal temperature variations, where they remain indefinitely. (c) Ice that was quickly buried retreats far slower than ice exposed to vacuum.
Paper: Gradual Sequestration of Water at Lunar Polar Conditions due to Temperature Cycles
Authors: Norbert Schorghofer
Figure caption: Fit of the BET isotherm to adsorption isotherm measurements. The vertical axis uses a combination of variables that turns the BET isotherm into a straight line. p0 is the saturation vapor pressure of water. The BET Equation (2) has only one free parameter. The measurements with the highest partial pressures were omitted from the fit, but nevertheless θ → ∞ as p → p0.
Paper: Gradual Sequestration of Water at Lunar Polar Conditions due to Temperature Cycles
Authors: Norbert Schorghofer
Figure caption: Temperature and equilibrium H2O concentration profiles as a function of depth at the study sites (a), (b) west of Nobile and (c), (d) west of Haworth. (a), (c) Mean, minimum, and maximum temperatures. (b), (d) Equilibrium H2O concentrations for two water delivery rates.
Paper: Gradual Sequestration of Water at Lunar Polar Conditions due to Temperature Cycles
Authors: Norbert Schorghofer
Figure caption: Result of microphysical model calculations at the study site west of Haworth Crater, with a delivery rate of 1000 kg m2 Gyr−1. (a) Histograms of H2O concentration in intervals of 10 kyr. (b) Column-integrated mass of sequestered H2O as a function of time. (c) Fraction of H2O sequestered as a function of time.
Paper: Detection of the S(1) Rotational Line of H2 toward IRC+10216: A Simultaneous Measurement of the Mass-loss Rate and CO Abundance
Authors: J. P. Fonfría, C. N. DeWitt, E. J. Montiel, J. Cernicharo, and M. J. Richter
Figure caption: H2 lines observed toward IRC+10216 (black histograms) and models (red curves). The model for the S(1) line is the best fit (see text). The gray spectra are the atmospheric transmission. The flights are given in green at the top right of each panel. F560 was the only flight where the S(1) line was not strongly blended with a close strong telluric line. The vertical dotted–dashed line at zero velocity represents the systemic velocity of IRC+10216 and the vertical gray dashed lines at ±14.5 km s−1 the terminal gas expansion velocity in front of and behind the star. The horizontal gray dashed lines are at the 3σ level.
Paper: Detection of the S(1) Rotational Line of H2 toward IRC+10216: A Simultaneous Measurement of the Mass-loss Rate and CO Abundance
Authors: J. P. Fonfría, C. N. DeWitt, E. J. Montiel, J. Cernicharo, and M. J. Richter
Figure caption: ISO/SWS observed and fitted continuum emission of IRC+10216 (black and red). The continuum emission calculated assuming no dust inwards from 5 R⋆ is plotted as a dashed blue curve. Molecular and solid state bands are indicated (e.g., Fonfría et al. 2021).
Paper: Detection of the S(1) Rotational Line of H2 toward IRC+10216: A Simultaneous Measurement of the Mass-loss Rate and CO Abundance
Authors: J. P. Fonfría, C. N. DeWitt, E. J. Montiel, J. Cernicharo, and M. J. Richter
Figure caption: Observed spectrum around the rest frequency of the S(1) line of ortho-H2 (labeled in red). The lines of C2H2 and HCN in this range are indicated in blue and green, respectively. Approximate spectra of HNC are plotted in orange and magenta (see text). The gray spectrum is the atmospheric transmission calculated with ATRAN (Lord 1992).
Paper: Detection of the S(1) Rotational Line of H2 toward IRC+10216: A Simultaneous Measurement of the Mass-loss Rate and CO Abundance
Authors: J. P. Fonfría, C. N. DeWitt, E. J. Montiel, J. Cernicharo, and M. J. Richter
Figure caption: Gas expansion velocity and kinetic temperature derived from the fit to the H2 S(1) line (black and red, respectively). The dashed blue curve is a fit to the gas expansion velocity assuming the theoretical profile for an expansion envelope driven by radiation pressure on dust grains (﹩{v}_{\exp }={v}_{\infty }{\left(1-{R}_{0}/r\right)}^{\beta }﹩, where v∞ = 14.4 km s−1, R0 = 1R⋆, and β = 2.4). The solid blue curve is the same but considering two different acceleration regimes (v∞,1 = 11.3 km s−1, R0,1 = 1R⋆, β1 = 1.6, v∞,2 = 5.2 km s−1, R0,2 = 7R⋆, and β2 = 2.2). The orange profile is a fit to TK assuming a power law. This quantity is uncertain in the range 1−5R⋆, shaded in gray (see text).
Paper: The Kiloparsec-scale Neutral Atomic Carbon Outflow in the Nearby Type 2 Seyfert Galaxy NGC 1068: Evidence for Negative AGN Feedback
Authors: Toshiki Saito, Shuro Takano, Nanase Harada, Taku Nakajima, Eva Schinnerer, Daizhong Liu, Akio Taniguchi, Takuma Izumi, Yumi Watanabe, Kazuharu Bamba, Eric Herbst, Kotaro Kohno, Yuri Nishimura, Sophia Stuber, Yoichi Tamura, and Tomoka Tosaki
Figure caption: (a) [C I](1–0) integrated intensity map of the central 1 kpc of NGC 1068 (FoV-1) at 0.″8 resolution (∼55 pc). The contours are (0.025, 0.05, 0.1, 0.2, 0.4, 0.8, and 0.96) × peak, where peak = 714 K km s−1. The two dashed lines crossing the AGN position (Roy et al. 1998) denote the approximate outer edges of the ionized gas cones (Mingozzi et al. 2019). The black circle indicates the FoV of the Band 8 12 m + 7 m data. (b) CO(1–0) integrated intensity map at 0.″8 resolution (T. Tosaki et al., in preparation). The [C I](1–0) contours are overlaid. (c) [C I](1–0)/CO(1–0) integrated intensity ratio map. (d) Pixel-by-pixel comparison between the [C I](1–0) and CO(1–0) maps. Pixel size is 0.″2 × 0.″2. Pixels within the cones in FoV-1 are colorized by their projected distance from the AGN position, and pixels outside the cones in FoV-1 are shown in black. Pixels in FoV-2 and FoV-3 (two positions in the starburst ring; Takano et al. in preparation) are shown in gray for reference.
Paper: The Kiloparsec-scale Neutral Atomic Carbon Outflow in the Nearby Type 2 Seyfert Galaxy NGC 1068: Evidence for Negative AGN Feedback
Authors: Toshiki Saito, Shuro Takano, Nanase Harada, Taku Nakajima, Eva Schinnerer, Daizhong Liu, Akio Taniguchi, Takuma Izumi, Yumi Watanabe, Kazuharu Bamba, Eric Herbst, Kotaro Kohno, Yuri Nishimura, Sophia Stuber, Yoichi Tamura, and Tomoka Tosaki
Figure caption: (a) [C I]/CO intensity ratio channel maps of NGC 1068. We show pixels with a lower limit of the ratio higher than unity in the reddest color (i.e., CO non-detected pixels but detected in [C I]). The left (right) panels show the blueshifted (redshifted) part from the systemic velocity. The relative velocity offset is larger in the upper panels. The [C I] contours are overlaid. (b) Channel maps of the truncated, decelerating bicone model. This simple model largely reproduces the kinematics of the observed high-ratio gas shown in red.
Paper: The Kiloparsec-scale Neutral Atomic Carbon Outflow in the Nearby Type 2 Seyfert Galaxy NGC 1068: Evidence for Negative AGN Feedback
Authors: Toshiki Saito, Shuro Takano, Nanase Harada, Taku Nakajima, Eva Schinnerer, Daizhong Liu, Akio Taniguchi, Takuma Izumi, Yumi Watanabe, Kazuharu Bamba, Eric Herbst, Kotaro Kohno, Yuri Nishimura, Sophia Stuber, Yoichi Tamura, and Tomoka Tosaki
Figure caption: Illustrations of the truncated, decelerating bicone model (model 3). (a) View from Earth. (b) View from the disk plane. The high-[C I]/CO-ratio gas is distributed within the red and blue parts (i.e., overlap regions between the bicone and the disk).
Paper: The Kiloparsec-scale Neutral Atomic Carbon Outflow in the Nearby Type 2 Seyfert Galaxy NGC 1068: Evidence for Negative AGN Feedback
Authors: Toshiki Saito, Shuro Takano, Nanase Harada, Taku Nakajima, Eva Schinnerer, Daizhong Liu, Akio Taniguchi, Takuma Izumi, Yumi Watanabe, Kazuharu Bamba, Eric Herbst, Kotaro Kohno, Yuri Nishimura, Sophia Stuber, Yoichi Tamura, and Tomoka Tosaki
Figure caption: (a) The constant bicone model with no truncation (model 1). (b) The decelerating bicone model with no truncation (model 2).
Paper: The Kiloparsec-scale Neutral Atomic Carbon Outflow in the Nearby Type 2 Seyfert Galaxy NGC 1068: Evidence for Negative AGN Feedback
Authors: Toshiki Saito, Shuro Takano, Nanase Harada, Taku Nakajima, Eva Schinnerer, Daizhong Liu, Akio Taniguchi, Takuma Izumi, Yumi Watanabe, Kazuharu Bamba, Eric Herbst, Kotaro Kohno, Yuri Nishimura, Sophia Stuber, Yoichi Tamura, and Tomoka Tosaki
Figure caption: (a) The [C I] outflow intensity map (see Appendix B). (b) HST [O III] map. (c) VLA 8.49 GHz continuum map. (d) VLT/MUSE [S III]/[S II] line ratio map (i.e., ionization parameter map). (e) Pixel-by-pixel comparison between the [C I](1–0)/CO(1–0) ratio and [S III]/[S II] ratio maps. Pixels within the cones in FoV-1 are color-coded by projected distance from the AGN, and pixels lying outside the cones in FoV-1 are shown in black. Pixels in FoV-2 and FoV-3 (i.e., starburst ring) are shown in gray. (f) [C I](1–0) and CO(1–0) spectra toward the bicone (top) and FoV-1 (bottom). We use the [C I]-detected pixels of Figure 5(a) when extracting the bicone spectra.
Paper: Gaia 0007–1605: An Old Triple System with an Inner Brown Dwarf–White Dwarf Binary and an Outer White Dwarf Companion
Authors: Alberto Rebassa-Mansergas, Siyi Xu, Roberto Raddi, Anna F. Pala, Enrique Solano, Santiago Torres, Francisco Jiménez-Esteban, and Patricia Cruz
Figure caption: Panel (a): the observed X-Shooter spectrum of Gaia 0007–1605 A,C (gray), the best-fit white dwarf model (blue) and its combination with a 2300 K and 5.0 dex CIFIST model (magenta; corresponding to a star of spectral type M9.5) and a 1900 K and 5.5 dex CIFIST model, i.e., the best fit to the observed spectrum. An M9.5 companion can clearly be ruled out, which confirms the near-infrared excess to arise from a brown dwarf. The structure at ≃14.000 Å and ≃19.000 Å is related to the residuals of the telluric correction. Panel (b): the same but for the optical range of the spectrum, where the white dwarf dominates the SED. Panel (c): the combined best fit to the near-infrared range of the spectrum. The effective temperature and surface gravity of the brown dwarf are indicated in the top-left corner and the dashed vertical line indicates the KI 12 432.27/12 522.14 Å absorption doublet from which we measure the radial velocity. Panels (d), (e), and (f): for comparison, we show the second-best (d), third-best (e), and fourth-best (f) CIFIST models superimposed on the observed near-infrared spectrum. The effective temperatures and surface gravities are also indicated.
Paper: Gaia 0007–1605: An Old Triple System with an Inner Brown Dwarf–White Dwarf Binary and an Outer White Dwarf Companion
Authors: Alberto Rebassa-Mansergas, Siyi Xu, Roberto Raddi, Anna F. Pala, Enrique Solano, Santiago Torres, Francisco Jiménez-Esteban, and Patricia Cruz
Figure caption: Top panel: Lomb–Scargle periodogram of the TESS light curve. The strongest signal at 1.0446 ± 0.0015 days exceeds the 1 and 0.1% false-alarm-probability (F. A. P.) thresholds. Middle panel: folded light curve, obtained from the 1.0446 day period. The black symbols are the binned light curve at 30 minute intervals, and the error bars represent the 1σ scatter in each bin. The blue sinusoidal curve corresponds to the detected periodic signal. Bottom panel: zoomed panel on the binned light curve.