adsabs/AstroCLIMB huggingface dataset:
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Histogram of the NB fluxes measured for all 533 SFACT candidates from the three pilot-study fields. We make no distinction between objects detected in the different NB filters. The median emission-line flux (denoted by the dashed vertical line) is 2.97 × 10−16 erg s−1 cm−2, while the sample appears to be substantially complete to ∼1.9 × 10−16 erg s−1 cm−2. The lower (black) histogram shows the distribution of NB fluxes for the 38 SFACT candidates that were found to be false detections in our follow-up spectroscopy (see Section 4.2).
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Histograms showing the g-band absolute magnitude distributions for the SFACT objects located in our pilot-study fields. The upper panel shows the M  g  distribution for the lower-redshift Hα-detected galaxies, while the middle and lower panels show the same distributions for the intermediate-redshift [O III]-selected galaxies and the [O II]-selected galaxies, respectively. In all three panels, the black-lined histogram plots the luminosity distribution for the full sample. The latter includes the higher-luminosity QSOs.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Example emission-line objects from the SFACT survey. Each row shows a trio of images: left is the BB continuum image, center is the NB image before continuum subtraction, and right is the continuum-subtracted NB image. Each image cutout shows a field of view of 50″ × 50″. Top: the spiral galaxy SFF10-NB1-C22247, which is marked by the lower set of red circles. Also indicated is the H II region SFF10-NB1-C22168. Middle: the faint (g = 24.98) source SFF15-NB2-D2938. Note how the object is dramatically brighter in the NB images. Bottom: the ELG SFF10-NB1-D11121. Spectra of all four SFACT sources illustrated in this figure are presented in Figure 5.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Histogram showing the redshift distribution of the SFACT ELGs. Only galaxies detected via their Hα, [O III], Hβ, [O II], and [Ne III] lines are included in the figure; higher-redshift QSOs are excluded. Unlike a typical magnitude-limited redshift survey, the SFACT survey samples the universe in discrete redshift windows
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Spectral plots of the objects illustrated in Figure 4. The y-axis plots the flux in erg s−1 cm−2 Å−1, while the x-axis shows the wavelength in angstrom units. The vertical red dashed lines found in all spectral plots presented in this paper indicate the FWHM bandwidth of the NB filter used to detect each object whose spectrum is shown. The upper row shows the spectra of both the central region (left) and an outlying H II region (right) for the spiral galaxy shown in the top image of Figure 4. The nuclear spectrum indicates that this object is an LINER. The lower row includes the spectrum of an [O III]-detected star-forming galaxy found in the NB2 filter (left), and a higher-redshift [O II]-detected system (right).
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Emission-line diagnostic diagram for the Hα-selected SFACT galaxies presented in the current paper. These objects are found in the redshift range z = 0.00–0.15. The different categories of emission-line sources are indicated by different symbols, as specified in the legend. The solid curve represents photoionization models from Dopita & Evans (1986), and the dashed curve shows the empirical demarkation line between AGN and star-forming galaxies from Kauffmann et al. (2003).
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Histogram showing the distribution of the star formation rates for the Hα-detected SFACT ELGs in the three pilot-study fields (n = 108). The object that stands out as having a low SFR is the sole Hα detection in the NB2 filter.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Spectrum of the cataclysmic variable (CV) star SFF17-NB2-D24012. This object was previously identified in a catalog of suspected CVs by Drake et al. (2014). It was detected in our survey due to the strong Hα emission located in NB2. Other lines visible in the spectrum include Hβ as well as five Helium lines: He I 4921, 5015, 5876, 6678, 7065. The lines are double peaked and broad, indicative of emission from a rapidly rotating disk.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Emission-line diagnostic diagram for the [O III]-selected SFACT galaxies presented in the current paper. These galaxies are found in the redshift range z = 0.30–0.52. The different types of emission-line sources are indicated by different symbols, as specified in the legend. The dashed line represents the trend line shown in Figure 1 of Baldwin et al. (1981).
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Spectrum of a candidate Green Pea galaxy SFF15-NB2-D22777. The combination of high equivalent width [O III] emission lines and high luminosity (M  g  = −19.3) is typical of the Green Peas.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Spectrum of the metal-poor dwarf galaxy SFF06-NB2-C4238. It has an estimated oxygen abundance log(O/H)+12 of 7.15 ± 0.10.
Paper: Measuring the Temperature of Starspots from Multi-filter Photometry
Authors: Maria C. Schutte, Leslie Hebb, John P. Wisniewski, Caleb I. Cañas, Jessica E. Libby-Roberts, Andrea S. J. Lin, Paul Robertson, Gumundur Stefánsson
Figure caption: Simulated light curves of binned LCO data in ﹩{g}^{{\prime} },{r}^{{\prime} },{i}^{{\prime} }﹩ and Zs bands (top left, top right, bottom left, and bottom right, respectively) compared to three STSP models corresponding to ﹩{{T}_{\mathrm{eff}}}_{{spot}}=﹩ 4300 K (blue line), 4500 K (orange line), and 4700 K (green line) with residuals of model—data shown for all three cases in bottom panel. In all cases the χ 2 of the STSP model compared to the simulated data is lowest for T eff = 4500 K though the two closest spot temperature models (4400 and 4600 K) fit within the Δ χ 2 of the 4500 K STSP model.
Paper: Measuring the Temperature of Starspots from Multi-filter Photometry
Authors: Maria C. Schutte, Leslie Hebb, John P. Wisniewski, Caleb I. Cañas, Jessica E. Libby-Roberts, Andrea S. J. Lin, Paul Robertson, Gumundur Stefánsson
Figure caption: Left column: data collected by MuSCAT3 instrument for HAT-P-11b transit obtained on 2021 June 29. The ﹩{g}^{{\prime} }﹩ band data are shown in the top panel with a precision of 0.58 mmag with an exposure time of 70 s. The ﹩{r}^{{\prime} }﹩ band data are shown below the ﹩{g}^{{\prime} }﹩ with a precision of 0.57 mmag with an exposure time of 40 s. The ﹩{i}^{{\prime} }﹩ band data are shown next with a precision of 0.62 mmag with an exposure time of 40 s. Lastly, the Zs band data are shown in the bottom panel with a precision of 0.54 mmag with an exposure time of 70 s. Right column: simulated light curves of LCO data in ﹩{g}^{{\prime} },{r}^{{\prime} },{i}^{{\prime} }﹩ and Zs bands from top to bottom panels, respectively, assuming the star was spotted as in the Kepler light curve in Figure 4. Black points correspond to simulated data with appropriate error bars. The no-spot transit model for each filter is shown as a cyan line with the residuals (no-spot model—simulated data) shown as black dots in bottom panel of each figure.
Paper: Measuring the Temperature of Starspots from Multi-filter Photometry
Authors: Maria C. Schutte, Leslie Hebb, John P. Wisniewski, Caleb I. Cañas, Jessica E. Libby-Roberts, Andrea S. J. Lin, Paul Robertson, Gumundur Stefánsson
Figure caption: Theoretical contrast values for HAT-P-11 assuming T eff = 4800 K and ﹩\mathrm{log}g=4.5﹩. A range of spot temperatures from 3700 to 4700 K in 100 K steps were used to calculate the contrast of the starspot for a range of filters. The contrast values are plotted as points at the filter’s central wavelength though the contrast applies to the entire bandpass. In order of central wavelength, the filters used were: SDSS ﹩{g}^{{\prime} }﹩, SDSS ﹩{r}^{{\prime} }﹩, Kepler, SDSS ﹩{i}^{{\prime} }﹩, TESS, OAO Zs, and SDSS ﹩{z}^{{\prime} }﹩. The solid black line at 0.3 corresponds to the area-weighted sunspot contrast assumed in Morris et al. (2017a) for their starspot modeling. The lines are colored by their spot temperature, with the coolest spots in cyan. The black star corresponds to the contrast value for magenta spot spectrum shown in Figure 1.
Paper: Measuring the Temperature of Starspots from Multi-filter Photometry
Authors: Maria C. Schutte, Leslie Hebb, John P. Wisniewski, Caleb I. Cañas, Jessica E. Libby-Roberts, Andrea S. J. Lin, Paul Robertson, Gumundur Stefánsson
Figure caption: Left: HAT-P-11's stellar photosphere spectrum with T eff = 4800 K and ﹩\mathrm{log}g=4.5﹩ in gray. Spectrum for spot temperature of 4500 K and ﹩\mathrm{log}g=4.5﹩ is shown in magenta. Spectra were obtained using the expecto Python package, which provides a PHOENIX model spectrum for the closest grid point for an input photospheric  temperature and surface gravity for solar metallicity stars. Right: the fluxes over which the spectra were integrated for the Kepler filter for the photosphere and spot are shown in filled-in hatches of gray and magenta, respectively. Once integrated over, the hatched regions correspond to the I spot (magenta) and I  phot  (gray) in Equation (1), which becomes a contrast of 0.32.
Paper: Measuring the Temperature of Starspots from Multi-filter Photometry
Authors: Maria C. Schutte, Leslie Hebb, John P. Wisniewski, Caleb I. Cañas, Jessica E. Libby-Roberts, Andrea S. J. Lin, Paul Robertson, Gumundur Stefánsson
Figure caption: Top: plot of the surface of HAT-P-11 with the final spot groups shown as black filled circles along with the red line denoting the equator of the star and with dashed lines denoting the full extent of the transit path for the secondary object (given ﹩\lambda \,=\,{106}_{-11}^{+15\circ }﹩). Bottom: light curve for final STSP fit (red line) along with the no-spot model for HAT-P-11 (cyan line) for chosen transit. The residuals (model—data) are shown below the light curve with black points.
Paper: Measuring the Temperature of Starspots from Multi-filter Photometry
Authors: Maria C. Schutte, Leslie Hebb, John P. Wisniewski, Caleb I. Cañas, Jessica E. Libby-Roberts, Andrea S. J. Lin, Paul Robertson, Gumundur Stefánsson
Figure caption: Starspot models using theoretical contrast curves assuming spot temperature of 3700 K for SDSS ﹩{g}^{{\prime} }﹩ (green line), SDSS ﹩{r}^{{\prime} }﹩ (red line), SDSS ﹩{i}^{{\prime} }﹩ (magenta line), and Zs (blue line) filters compared to Kepler data (black points) and the no-spot transit model (cyan line). This spot temperature assumes the spot temperature difference vs photosphere temperature model from Herbst et al. (2021). This spot temperature produces too-dark spots (bumps are too big) to fit the data.
Paper: Measuring the Temperature of Starspots from Multi-filter Photometry
Authors: Maria C. Schutte, Leslie Hebb, John P. Wisniewski, Caleb I. Cañas, Jessica E. Libby-Roberts, Andrea S. J. Lin, Paul Robertson, Gumundur Stefánsson
Figure caption: Starspot models using theoretical contrast curves assuming spot temperature of 4500 K for SDSS ﹩{g}^{{\prime} }﹩ (green line), SDSS ﹩{r}^{{\prime} }﹩ (red line), SDSS ﹩{i}^{{\prime} }﹩ (magenta line), Kepler (yellow line), and Zs (blue line) filters compared to Kepler data (black points) and the no-spot transit model (cyan line). This spot temperature fits the Kepler data best and corresponds to a contrast of 0.32 in the Kepler band, similar to the value of 0.3 assumed in Morris et al. (2017a).
Paper: Measuring the Temperature of Starspots from Multi-filter Photometry
Authors: Maria C. Schutte, Leslie Hebb, John P. Wisniewski, Caleb I. Cañas, Jessica E. Libby-Roberts, Andrea S. J. Lin, Paul Robertson, Gumundur Stefánsson
Figure caption: Data from LCO MuSCAT3 from HAT-P-11b transit on 2021 June 29 binned to 200 s for SDSS ﹩{r}^{{\prime} }﹩ (red) and SDSS ﹩{i}^{{\prime} }﹩ (magenta) and 210 s for SDSS ﹩{g}^{{\prime} }﹩ (green) and Zs (blue), with all filters plotted on top of each other. The bottom panel shows the residuals of the no-spot model for that filter minus the binned data points (cyan line here shows example no-spot model for SDSS ﹩{r}^{{\prime} }﹩).
Paper: The High-energy Spectrum of the Young Planet Host V1298 Tau
Authors: Girish M. Duvvuri, P. Wilson Cauley, Fernando Cruz Aguirre, Roy Kilgard, Kevin France, Zachory K. Berta-Thompson, J. Sebastian Pineda
Figure caption: The differential emission measure model fit compared to representative average DEM values derived from the observed fluxes used to constrain the fit. The uncertainty of allowed DEM shapes is greatest in the interval between 3 × 105 K and 3 × 106 K where there are no observed emission features formed at specifically those temperatures. The peak at 6 × 106 K corresponds to the corona and the DEM turning down prevents the formation of emission lines at temperatures greater than 1.5 × 107 K, which is consistent with the isothermal XSPEC model fit to the X-ray data. Figure 6 compares the fluxes predicted by the DEM model to the observed flux constraints.
Paper: The High-energy Spectrum of the Young Planet Host V1298 Tau
Authors: Girish M. Duvvuri, P. Wilson Cauley, Fernando Cruz Aguirre, Roy Kilgard, Kevin France, Zachory K. Berta-Thompson, J. Sebastian Pineda
Figure caption: The composite spectrum is plotted with each component covering a specific wavelength interval at its original wavelength resolution, using data where available and supplemented by empirically constrained models. The components and their respective wavelength intervals are: XSPEC model (gray), 1–100 Å; Differential emission measure model (light blue), 100–1150 Å; HST COS data (pink), 1150–1700 Å, with two sub-intervals 1214.63–1216.78 Å (Lyα) and 1519.42–1530.78 Å replaced with scaled excerpts from the MUSCLES SED for ϵ Eridani; HST STIS data (green), 1700–3100 Å; PHOENIX model (light brown), 3100–105 Å.(The data used to create this figure are available.)
Paper: The High-energy Spectrum of the Young Planet Host V1298 Tau
Authors: Girish M. Duvvuri, P. Wilson Cauley, Fernando Cruz Aguirre, Roy Kilgard, Kevin France, Zachory K. Berta-Thompson, J. Sebastian Pineda
Figure caption: The NICER spectrum from the October 2020 observation is plotted as blue circles with error bars while the best-fit XSPEC model is plotted in solid orange. The model fits the continuum and strong emission lines at intermediate energies well but is less consistent with the emission from low energies.
Paper: The High-energy Spectrum of the Young Planet Host V1298 Tau
Authors: Girish M. Duvvuri, P. Wilson Cauley, Fernando Cruz Aguirre, Roy Kilgard, Kevin France, Zachory K. Berta-Thompson, J. Sebastian Pineda
Figure caption: Lyα airglow subtraction of V1298 Tau. The spectrum as observed by COS is shown in dark blue. The CA23 tool is used to subtract the airglow, resulting in the recovered (ISM attenuated) spectrum in light blue. The recovered signal of V1298 Tau is faint, and a reliable reconstruction of the stellar emission was not possible.
Paper: The High-energy Spectrum of the Young Planet Host V1298 Tau
Authors: Girish M. Duvvuri, P. Wilson Cauley, Fernando Cruz Aguirre, Roy Kilgard, Kevin France, Zachory K. Berta-Thompson, J. Sebastian Pineda
Figure caption: The C IV doublet from V1298 Tau. COS/G160M spectra are shown as the black histogram, with representative error bars in red. A two-component Gaussian fit is shown overplotted; individual components are in the dashed magenta lines and the overall fit is in solid blue.
Paper: The High-energy Spectrum of the Young Planet Host V1298 Tau
Authors: Girish M. Duvvuri, P. Wilson Cauley, Fernando Cruz Aguirre, Roy Kilgard, Kevin France, Zachory K. Berta-Thompson, J. Sebastian Pineda
Figure caption: Both panels plot the planet radius against the orbital period for: a sample of confirmed exoplanets orbiting stars with a mass similar to V1298 Tau (translucent dots), the V1298 Tau planets (opaque circles), and solar system planets (opaque triangles). The top panel colors the planet markers by the age of the star, with darker shades representing young systems and increasing brightness with age, while the bottom panel colors the planet markers by the cumulative XUV irradiation experienced by the planet (F ⋆ is the flux received by the planet) assuming it has stayed at its current orbit for the entirety of the system’s age, with the brightness of the color increasing with irradiation. For this sample selected by stellar mass, where all plotted planets are assumed to have experienced the same high-energy evolution, the cumulative XUV irradiation is a function of age. In a broader sample, where different stellar hosts follow different XUV irradiation evolution behavior, the cumulative XUV irradiation will also depend on other parameters like stellar mass.
Paper: The High-energy Spectrum of the Young Planet Host V1298 Tau
Authors: Girish M. Duvvuri, P. Wilson Cauley, Fernando Cruz Aguirre, Roy Kilgard, Kevin France, Zachory K. Berta-Thompson, J. Sebastian Pineda
Figure caption: The observed flux constraints are plotted as black points with error bars corresponding to their measurement uncertainties while the DEM model predictions are plotted as light blue crosses with error bars corresponding to the 16th–84th percentile values of the distribution of fluxes predicted by drawing from the posterior of DEM shapes and the fractional flux systematic uncertainty parameter. The flux constraints are divided into two categories: ion species corresponding to integrated FUV emission line fluxes (labeled in pink) and central energies corresponding to the integrated flux of X-ray spectral bins (labeled in gray). Beneath each flux constraint’s label is its ﹩{\mathrm{log}}_{10}\left({T}_{\mathrm{formation}}\,[{\rm{K}}]\right)﹩ value and the constraints are ordered by formation temperature increasing to the right.
Paper: The High-energy Spectrum of the Young Planet Host V1298 Tau
Authors: Girish M. Duvvuri, P. Wilson Cauley, Fernando Cruz Aguirre, Roy Kilgard, Kevin France, Zachory K. Berta-Thompson, J. Sebastian Pineda
Figure caption: The broken-power laws describing the evolution of high-energy emission for solar-mass stars divided into 4 bandpasses, annotated with the time corresponding to the breakpoint of the power law: 1–20 Å (dashed dark blue; 52.9 Myr), 20–100 Å (solid orange, 24.2 Myr), 100–360 Å (dotted–dashed green, 108.7 Myr), 360–920 Å (dotted red; 35.9 Myr). The parameters for the broken-power laws are listed in Table 6.
Paper: The High-energy Spectrum of the Young Planet Host V1298 Tau
Authors: Girish M. Duvvuri, P. Wilson Cauley, Fernando Cruz Aguirre, Roy Kilgard, Kevin France, Zachory K. Berta-Thompson, J. Sebastian Pineda
Figure caption: The EUV spectrum of V1298 Tau (light blue) compared to the EUV spectrum of the quiescent Sun (Woods et al. 2009). The EUV spectrum of younger, more active V1298 Tau is consistently a factor of 100–1000 greater than the Sun’s across this wavelength regime, with a shallower slope for the H I continuum blueward of 912 Å  forming the base of the strong emission lines.
Paper: Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs
Authors: Aaron M. Meisner, S. K. Leggett, Sarah E. Logsdon, Adam C. Schneider, Pascal Tremblin, Mark Phillips
Figure caption: Color–color plots for T and Y dwarfs. The upward blue triangle (blue square) is the metal-poor benchmark T dwarf Wolf 1130C (Ross 19B). These two benchmark systems have metallicities of −0.75 and −0.40 dex, respectively (see Sections 2.1 and 2.2). Red points are (candidate) metal-poor brown dwarfs, identified by red text annotations in the bottom two panels. Red points with surrounding yellow stars represent objects for which we present new Gemini photometry. The gray lines connecting filled gray circles are solar-metallicity model sequences with log g = 4.5; the dots indicate the colors for the T eff values shown along the top axis. Light blue lines are also solar-metallicity sequences, but these have a higher gravity of log g = 5.0, implying a higher mass and older age for a given T eff (e.g., Figure 10 of Marley et al. 2021). Light green lines have log g = 4.5 and a metallicity of one-tenth solar. Gray dashed lines between the gray and blue sequences indicate the effect of increasing gravity at constant T eff, and gray solid lines between the gray and green sequences indicate the effect of decreasing metallicity at constant T eff. See Section 4.1 for a description of the models used in this figure, and Section 4.2 for a discussion of the observed trends.
Paper: Exploring the Extremes: Characterizing a New Population of Old and Cold Brown Dwarfs
Authors: Aaron M. Meisner, S. K. Leggett, Sarah E. Logsdon, Adam C. Schneider, Pascal Tremblin, Mark Phillips
Figure caption: Color–magnitude plots for T and Y dwarfs. The upward blue triangle (blue square) is the metal-poor benchmark T dwarf Wolf 1130C (Ross 19B). Outliers are identified. We present new J-band photometry for WISEA 1534−1043 in this work (red dot with surrounding yellow star). Red dots without a yellow star are data points from the prior literature for metal-poor brown dwarf candidates. The black arrow in the bottom panel illustrates the lower limit on J − W2 from Bardalez Gagliuffi et al. (2020) for WISEA 0830+2837. J0212+0531 is CWISEP J021243.55+053147.2 (Meisner et al. 2020a; Leggett et al. 2021). J0535−7500 is WISE J053516.80−750024.9 (Kirkpatrick et al. 2012). J1828+2650 is WISEPA J182831.08+265037.8 (Cushing et al. 2011; Kirkpatrick et al. 2011). Model sequences are shown as gray, blue, and green lines, as described in Figure 2. Gray filled circles on the gray sequence correspond to the colors for the T eff values shown on the left and right axes in the lower panel.