adsabs/AstroCLIMB huggingface dataset:
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Output of the spatially resolved SED fit on NGC 1614. The top row, from left to right, shows the RGB image (built combining the F435W, F814W, and F110W broadband filters), the stellar mass density map, and the SFRD maps inferred with the stellar continuum and with the Paβ emission-line flux. The bottom row shows the resulting Hα and Paβ surface density flux maps, as well as the A  V  inferred from the empirical Balmer-to-Paschen decrement, and the stellar continuum.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Histograms of the [N II]/Hα ratio for the six galaxies that are part of the GOALS survey, as measured in the MUSE IFU cube. The value we adopt for the ratio is indicated with a black dashed line on the histogram, and the gray shaded region shows the 1σ interval around of the mean. The y-axis is normalized.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Spatially resolved visual extinction inferred from the Balmer decrement (left) and SFRD inferred from the dust-corrected Paβ (right) vs. the visual extinction from the Balmer-to-Paschen decrement. The color code indicates the A  V  inferred with the classic Balmer decrement.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Top: maps of the Hα line flux for target MCG-02-01-051 inferred with only HST photometry (left), and with HST and extra synthetic photometry from MUSE (right). Bottom: ratio of both Hα estimates in each spatial bin. The running median and scatter are shown as a solid black line and surrounding shaded region, respectively.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Top: set of continuum templates that we use in our SED fitting code. Bottom: Hα+[N II] (left) and Paβ (right) pure line emission templates.
Paper: GWFAST: A Fisher Information Matrix Python Code for Third-generation Gravitational-wave Detectors
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Flowchart of the functioning of GWFAST. See Section 2.1 for the description of the inputs.
Paper: GWFAST: A Fisher Information Matrix Python Code for Third-generation Gravitational-wave Detectors
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Comparison of the waveform models TaylorF2_RestrictedPN (left panel), IMRPhenomD (central panel), and IMRPhenomD_NRTidalv2 (right panel) obtained from LAL and GWFAST—WF4Py for example events. The upper and central panels of both figures show the “+” GW amplitude and cosine of the phase obtained with the two codes superimposed, while in the lower panel, we report the relative difference (“residual”) among the two amplitudes.
Paper: GWFAST: A Fisher Information Matrix Python Code for Third-generation Gravitational-wave Detectors
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: The same as in Figure 2 for the waveform models IMRPhenomHM (left panel), IMRPhenomNSBH (central panel), and IMRPhenomXAS (right panel).
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: The mean and dispersion (not the uncertainty on the mean) of the per-star changes in synthetic photometry for different analysis variants compared to our primary calibration to 14 CALSPEC stars, with the inclusion of nightly SNIFS temperature coefficients. The small black points indicate the changes if we regress on time of night instead of temperature (i.e., replace ΔT with Δdate in Equation (5)). This has essentially no effect on the recovered standard-star fluxes (changes are ∼1 mmag), indicating that there is no evidence of changes in the SNIFS calibration during each night that are not driven by temperature changes. The red triangles show our original unblinded calibration: calibrated to CALSPEC but with no nightly SNIFS temperature coefficients. The mean star essentially does not change (indicating good mixing of primary and secondary stars through each night), but scatter of several millimagnitudes from star to star is seen in the U band. Next, the green points show the results from calibrating to the three fundamental CALSPEC white-dwarf models directly (with STIS observations not used at all) with no nightly SNIFS temperature coefficients. We see a shift of ∼5 mmags in the U and B bands, with the same several millimagnitude scatter from star to star. Finally, the blue squares show the three-white-dwarf calibration, but with temperature coefficients. The U and B offsets decrease somewhat, and the star-to-star scatter drops to 1–2 mmags. This indicates that some of the original tension we saw between the three-white-dwarf calibration and the CALSPEC calibration is due to when in the night the white dwarfs tended to be observed. Importantly, it also indicates that our network is rigid, and that changing the primary calibration stars moves the entire network together (at least if nightly temporal or temperature coefficients are used). As for the remaining difference between the CALSPEC observations and models for the three WD fundamental calibrators, it is in line with the disagreement shown around the Balmer jump in Figure 9 of Bohlin et al. (2020).
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: The Δm  l  values for each star showing the offset with respect to CALSPEC. On the left, we show the full Δm  l  for each star, making plain that most of the power is in the form of constant-in-wavelength offsets. On the right, we have removed the constant term in order to highlight the chromatic components. The vertical blue-shaded region shows the SNIFS dichroic crossover wavelength range; there does not appear to be much structure between the blue and red sides of SNIFS. The vertical magenta-shaded band is the region where the CALSPEC HST observations change grating coverage. The values have been median-smoothed in wavelength for clarity. Only primary calibrators observed on more than one night are shown, since otherwise the per-observation repeatability dominates, forcing the Δ m  l  to fall back on the prior, σ  l .
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: The airmass-dependent term, k, plotted vs. wavelength for our primary (extinction linear in airmass) analysis. For comparison purposes, we have added the 20 mmag gray instrumental component discussed in Section 5.2. The blue line is the mean k, and the blue band is the inferred rms of the night-to-night variation in k. Major atmospheric features are marked, as is the wavelength range of the SNIFS dichroic crossover. A physical atmospheric model, updated from Buton et al. (2013) to include updated ozone cross sections from Serdyuchenko et al. (2014) and a 40% reduction in the amount of aerosol scattering, is shown as the red dashed line. (Note that Buton et al. 2013 modeled telluric lines in a separate step, so for their curve, the telluric features are not included.) We see overall good agreement between our wavelength-by-wavelength model and a physical model. Note that no smoothness constraint in wavelength is imposed, so this agreement is an excellent cross-check.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Comparison of the expected and measured corrections to place the SSPS sample on the CALSPEC system. The upper panel shows the CALSPEC spectrum of Vega with the Hayes (1985) flux values overlaid. The red squares represent the wavelength bins, originally defined by Taylor (1984), used to establish the calibration for the SSPS sample by Hamuy et al. (1992, 1994). This illustrates the difficulties around the Balmer and Paschen absorption lines that needed to be avoided for the original SSPS calibration. (Note that the Taylor 1984 bin around 8700 Å was not used for SSPS calibration.) The lower panel shows the expected ratio of Hayes (1985) to CALSPEC (light-red squares), our mean measured ratio between the original SSPS spectra and our recalibration (light-blue line, with a cyan band representing the standard deviation among our sample of the SSPS stars), and our ratios at the SSPS/Taylor (1984) wavelengths (black points, with uncertainties in mean along the ratio axis and the width range along the wavelength axis). Our ratios are higher than the prediction, i.e., the original SSPS spectra gave fluxes higher than for the CALSPEC system, by around 1.8%.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: The inferred repeatability floor (left) and observed outlier fractions (right) vs. wavelength from our robust Bayesian hierarchical calibration model. To improve the signal-to-noise ratio, we show these results binned in 40-wavelength bins. The repeatability is obviously much better for long exposures than for short exposures, and the outliers occur more frequently for short exposures as well. See Section 5.5 for a detailed discussion.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: The dispersion of the Δm values (σ  l  from Equation (4)) for our 14 CALSPEC standards (black curve). The calculation is performed in bins of 40 wavelength samples in order to lower the uncertainty on the individual Δm values for stars with fewer (STIS and/or SNIFS) observations. Overplotted are the dispersions when comparing filter photometry for the UBVRI filters (Bohlin & Landolt 2015; BL15 magenta diamonds). We have updated the UBVRI intrinsic dispersion, including subtraction of the quoted filter photometry measurement uncertainty, to include newer space-based CALSPEC standard stars (green squares). We also plot a similar comparison that we have done for Pan-STARRS1 in the griz filters. These points have been offset slightly in wavelength for clarity. This demonstrates that the dispersion of Δ m values determined from our Bayesian hierarchical standardization model are consistent with other external checks of CALSPEC.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: We show eigenvectors constructed from the star-to-star covariance of the mean flux of each star averaged across 4000–7000 Å (to improve signal-to-noise ratio compared to a single wavelength). The off-diagonal elements of the covariance matrix are decomposed into first one eigenvector (shown in the top panel) and then after removing the outer product of that vector with itself, the remaining off-diagonal covariance matrix is decomposed into the next vector (shown in the bottom panel). The linear size of the plot points indicates the inverse uncertainty of each star. The first eigenvector is nearly constant from star to star, and the ∼2.5 mmag scale indicates the high precision of the match of our network to CALSPEC. Our model naturally gives this uncertainty from the number of CALSPEC stars, the number of observations, the estimated internal consistency of our network vs. CALSPEC, the repeatability of SNIFS, and the signal-to-noise ratio of the observations. The second vector shows very small (∼1 mmag) correlations on the sky.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: This figure shows a robust decomposition of the per-spectrum residuals (as a function of wavelength) into eigenvectors to investigate the repeatability floor seen in Figure 11. We show the first three eigenvectors here; these explain more than 90% of the variance. Each eigenvector is multiplied by the square root of the eigenvalue, so that the amount of dispersion is shown (in millimagnitude). The first eigenvector is mostly gray and explains about 5/6 s of the variance. The second eigenvector introduces a small tilt with wavelength with a peak-to-peak size of ∼14 mmags. The third eigenvector shows curvature and a small amount of H2O variation, with a peak-to-peak size of ∼12 mmags.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: The results of our leave-one-out test. The calibration model has been rerun for each primary standard star, moving that star to a secondary standard. We plot the change (in millimagnitude) from our calibration of the star when it is a primary to our calibration when it is a secondary. For better signal-to-noise ratio, we again bin in wavelength. Overall, our network is robust to the loss of any one primary standard star. We do not show HD 31128 and HD 74000 because they have few measurements, and thus their measurement uncertainties are dominated by repeatability.
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for Mg+ lines at 2796.35 Å and 2803.53 Å and (b) the solar spectrum utilized in the region of the lines. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for Mg+.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the three S I lines at 1807.31, 1820.34, and 1826.25 Å and (b) the solar spectrum utilized in the region of the lines. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The SORCE SOLSTICE high-resolution spectrum was used for S, with the date corresponding to 2009 March 1 (prior to the power-cycling issues that began in 2010). The spectral data were obtained from the LASP LISIRD website.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the three FUV O I lines at 1302.17, 1304.86, and 1306.03 Å, respectively, and (b) the solar spectrum utilized in the region of the lines. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). For the oxygen triplet lines between 1302 and 1306 Å, we generated line-shape profiles according to Gladstone (1992) and then scaled them to the appropriate irradiance levels in the same SORCE SOLSTICE spectrum used for the sulfur triplet lines.(The data used to create this figure are available.)
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Histograms showing the incidence of standard-star observations per airmass (left) and airmass range (right). The values are color coded by the sample—primary (blue) or secondary (magenta)—to which each standard star or pair of standard stars belongs. For the airmass range calculation, a pair is categorized as “primary” if at least one star in the pair is one of our primary standard stars. These distributions demonstrate that the airmass values and ranges are very similar for the primary (space-based CALSPEC) and secondary (SSPS; Oke 1990) standard stars.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Array showing the number of times different pairs of stars were observed on the same photometric night. The stars are ordered by R.A. and color coded (primary CALSPEC in blue, long-exposure secondaries in magenta, and short-exposure secondaries in red). Four stars observed on fewer than five nights are included in our analysis, but removed from this figure for clarity. Note that the plot is symmetric. Some seasonal structure exists, but overall our standard-star network is knit together quite well. Groupings of bright and faint stars result from our method for observing standard stars during twilight, with brighter stars observed when twilight is brighter and fainter stars observed when twilight is fainter or between the end and start of astronomical twilight.