adsabs/AstroCLIMB huggingface dataset:
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: CMDs of Czernik 41 (a)–(b) and NGC 1342 (c)–(d) in the UBV ((a) and (c)) and Gaia ((b) and (d)) photometric systems. Gray circles represent stars with membership probabilities P < 0.5, while colored circles indicate stars with P ≥ 0.5. The continuous and dashed blue curves denote the ZAMS lines used to define the cluster main sequences (H. Sung et al. 2013).
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: Star fields for Czernik 41 (a) and NGC 1342 (b) in the equatorial coordinate system. The red boundaries indicate the fields observed with the T100 telescope. North and east correspond to the up and left directions, respectively.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: King profiles of Czernik 41 (a) and NGC 1342 (b). The black solid curves represent the best-fit models, while the shaded red and gray regions indicate the confidence intervals of the model and the background stellar density, respectively. The dashed vertical lines denote the limit radii of the OCs.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: Histograms of stars in Czernik 41 (panels (a) and (b)) and NGC 1342 (panels (c) and (d)) as a function of V and G magnitudes. The black dashed lines show the photometric completeness limits for each band. The blue and red color bins represent the observed and the Besançon Galaxy model values, respectively.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: Czernik 41 (a)–(b) and NGC 1342 (c)–(d) OC fields: Gaia DR3 PM components (left panels) and sky orientation vectors in equatorial coordinates (right panels). The color scale and circles are identical to Figure 4. Black plus signs in panels (b) and (d) denote the central equatorial coordinates of the OCs.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: Membership probability distributions for all stars detected in the cluster fields of Czernik 41 (a) and NGC 1342 (b), constructed for Gaia data. The filled gray histograms represent the membership probabilities of all stars identified within the cluster fields, while the filled blue histograms correspond to stars within the limit radius (﹩{r}_{{\rm{lim}}}\,\leqslant \,1{1}^{{\prime} }﹩).
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: Trigonometric parallax histograms for the members of Czernik 41 (a) and NGC 1342 (b) within the limiting radius (﹩{r}_{{\rm{lim}}}\,\leqslant \,1{1}^{{\prime} }﹩) and with a relative parallax error of σϖ/ϖ < 0.2. The Gaussian functions applied to the distributions are shown as dashed red lines.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The cumulative radial distribution of stars across various mass ranges for Czernik 41 (a) and NGC 1342 (b).
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption: Normalized transit lightcurves from MuSCAT3 in the g, r, i, and z passbands. The top row shows both the lightcurve model (black, dashed lines) and the Gaussian process used to account for the systematics (orange line).
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption: Comparison of radial velocities derived from the red and blue arms of MAROON-X. Points in red are discrepant at the 2﹩\sqrt{{\sigma }_{\rm{Red}\,}^{2}+{\sigma }_{\,\rm{Blue}}^{2}}﹩ level; however, we found no additional reason to exclude these points from the analysis.
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption: Transit timing variations for TOI-1759A b from 12 TESS transits. The shaded blue area represents the 1σ spread (2.8 minutes), which is comparable to the cadence of the TESS photometry (2 minutes).
Paper: Dynamical Analysis of the HD 169142 Planet-forming Disk: Twelve Years of High-contrast Polarimetry
Authors: Miles Lucas, Michael Bottom, Ruobing Dong, 董若冰, Myriam Benisty, Mario Flock, Maria Vincent, Jonathan Williams, Kyohoon Ahn, Thayne Currie, Vincent Deo, Olivier Guyon, Tomoyuki Kudo, Lucinda Lilley, Julien Lozi, Maxwell Millar-Blanchaer, Barnaby Norris, Sebastián Pérez, Boris Safonov, Peter Tuthill, Taichi Uyama, Sébastien Vievard, Manxuan Zhang
Figure caption: Schematic diagram of the HD169142 disk. The black contours are based on the ALMA 1.3 mm continuum data, which trace out the warped inner envelope (B0), inner cavity (D1), a close inner ring (B1), a ring gap (D2), and three outer rings (B2–B4) with intermediate gaps (D3, D4). The red contours are based on visible-to-near-IR scattered light images, separated into an inner and outer ring. The location of the candidate protoplanet HD 169142 b from I. Hammond et al. (2023) is marked with a circled cross.
Paper: LEO-Vetter: Fully Automated Flux- and Pixel-level Vetting of TESS Planet Candidates to Support Occurrence Rates
Authors: Michelle Kunimoto, Steve Bryson, Drayson Jaffee, Jason F. Rowe, Tansu Daylan, Steven Giacalone, Jack J. Lissauer, Michael R. B. Matesic, Susan E. Mullally, Yoshi Nike Emilia Eschen
Figure caption: Period–radius diagram of systematics-dominated observed TCEs (left) and only PCs passing both flux- and pixel-level vetting (right). The properties of observed TCEs were estimated using the simple LEO-Vetter-implemented transit-model fits, while the properties of PCs were estimated using more comprehensive transit modeling (Section 7.1). PCs are color coded by their reliability against astrophysical false positives (Section 7.2), where higher values mean that the candidate is more likely to be a real planet. However, reliability will not be robust for planets larger than Rp = 8 R⊕ (dotted gray line) due to degeneracies with brown dwarfs and low-mass stars (S. Giacalone et al. 2021).
Paper: LEO-Vetter: Fully Automated Flux- and Pixel-level Vetting of TESS Planet Candidates to Support Occurrence Rates
Authors: Michelle Kunimoto, Steve Bryson, Drayson Jaffee, Jason F. Rowe, Tansu Daylan, Steven Giacalone, Jack J. Lissauer, Michael R. B. Matesic, Susan E. Mullally, Yoshi Nike Emilia Eschen
Figure caption: Promising PCs identified by LEO-Vetter that are not yet TOIs. The 13 PCs that are new CTOIs as a result of this work are indicated by the label “New.” The rest are known CTOIs from other works (M. Montalto et al. 2020; D. L. Feliz et al. 2021; Y. N. E. Eschen & M. Kunimoto 2024; J. D. Hartman et al. 2024). Gray dots show the underlying TESS data, while blue dots show the data binned every 15 minutes.
Paper: LEO-Vetter: Fully Automated Flux- and Pixel-level Vetting of TESS Planet Candidates to Support Occurrence Rates
Authors: Michelle Kunimoto, Steve Bryson, Drayson Jaffee, Jason F. Rowe, Tansu Daylan, Steven Giacalone, Jack J. Lissauer, Michael R. B. Matesic, Susan E. Mullally, Yoshi Nike Emilia Eschen
Figure caption: An example of the analysis described in Section 7.3, demonstrating the standard deviation of the MES metric as a function of period and MES. There is a similar grid for every metric.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Periodogram data for TESS SPOC TCE TIC 232568235-1-S24 (TOI 2260.01, CP) after preprocessing, as described in Section 4.2, without normalization. The figures display the flux and transit model periodograms. TOI 2260.01 is classified as a CP orbiting a variable star. The red dashed lines indicate the estimated periods of a double-sinusoidal function fitted to the photometric variability of TIC 232568235, derived from T. Fetherolf et al. (2023).
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Preprocessed difference image data for TESS SPOC TCE TIC 82707763-1-S37 (TOI 1046.01, an NEB), following the steps outlined in Section 4.2 without normalization. From left to right, the panels display the difference image, the out-of-transit image, and the target position image. In the difference and out-of-transit images, the red cross marks the location of the target, TIC 309787037, with its coordinates mapped to the CCD frame. In the target position image, the pixel containing the target is highlighted in yellow.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: The top and bottom figures show the phase-folded, binned trend and detrended flux time series for TESS SPOC TCE TIC 167526485-1-S6 (classified as an EB in A. Prša et al. 2022), respectively, without normalization. The red dashed lines indicate the estimated transit duration for this TCE, centered around the estimated transit midpoint.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Kepler vs. TESS histograms of MES with a focus on values >10 for exoplanets (KP+CP) and AFPs (EB+FP+BD).
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Unfolded binned flux data for TESS SPOC TCE TIC 98545929-1-S1-36 (TOI 1916.01, KP). The red dashed lines highlight the transit duration estimate of the detected TCE (∼3.68 hr) centered on the estimated transit midpoint.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Score distribution vs. orbital period (top) and planet radius (bottom) of non-exoplanet categories for the TESS+Kepler-aggregate model. Note: the width of bars does not carry any meaning.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: PR curve and confidence of different models.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Kepler vs. TESS histograms of large values of MES for exoplanets (KP+CP) and AFPs (EB+FP+BD).
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Precision and recall heatmaps as functions of MES, orbital period (days), and planet radius (Earth radii).
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: A schematic depicting the data reduction process using a sample spectrum from observations of HIP 67522 b. We represent the continuum-normalized raw data in black, the telluric model in red, the telluric-corrected data in orange, and the continuum-normalized telluric and stellar-corrected data in green. All steps in the reduction process depicted are offset by a scalar for better visualization. The region of integration used for HIP 67522 b is noted by the vertical blue lines.
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: The young planet population in period-radius space. The color denotes the age of the planet. HIP 67522 b is marked by a diamond, DS Tuc A b by a cross, and HD 63433 b by a star. The contours indicate the relative occurrence of planets inferred from the Kepler distribution (A. Dattilo et al. 2023). The young planet population shown is not corrected for completeness, although young planets are known to be larger than their older counterparts even after accounting detection biases (S. Vach et al. 2024).
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: The time evolution of the reduced and template-corrected spectra for HIP 67522 b spanning observations on 2021 May 14 UT. The color bar shows the time of observation relative to the predicted midpoint of the transit. The lines in red denote ingress and egress. The vertical dashed lines mark the region used to calculate the equivalent widths.
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: Same as Figure 3 but for HD 63433 b observations taken on 2020 March 7 UT.
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: Same as Figure 3 but for DS Tuc A b observations taken on 2019 October 7 UT.
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: Same as Figure 3 but for DS Tuc A b observations taken on 2019 August 19 UT.
Paper: Toward a 2D H I Map of the Local Interstellar Medium
Authors: Allison Youngblood, Kevin France, Tommi Koskinen, James Paul Mason, Seth Redfield, Brian E. Wood, Vincent Bourrier, Leonardo dos Santos, Christopher Johns-Krull, George W. King, Jeffrey L. Linsky, Sarah Peacock
Figure caption: The contour plot shows, for the Earth’s atmosphere, the specific energy input (qE) of primary photoelectrons normalized by the peak of this energy input (﹩{q}_{{\rm{E}},{\rm{\max }}}﹩) as a function of wavelength and altitude. This would represent the photoelectron heating rate for 100% heating efficiency. In reality, the heating efficiency depends on atmospheric properties. An NRLMSIS atmosphere at 60° solar zenith angle and noon local time and a TIMED/SEE solar spectrum at moderate activity were used. The horizontal dotted line at ∼120 km demarcates the altitude above which heating dominates and escape occurs. This figure illustrates the relative importance of different wavelength regions to the EUV energy input.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: Examples of the (a) RI and (b) NGI methods. The location of the injected source is marked with a red dot. (a) The RI method yields injected sources relatively isolated from other point sources. (b) The top example shows the injected source located approximately 4″ away from the center of its associated galaxy, which is a relatively short distance. In contrast, the bottom example shows an injected source associated with a large galaxy. Since the injection coordinates are determined based on the galaxy size, the source is placed relatively far from the galaxy's center, at a distance of approximately 19″.
Paper: Toward a 2D H I Map of the Local Interstellar Medium
Authors: Allison Youngblood, Kevin France, Tommi Koskinen, James Paul Mason, Seth Redfield, Brian E. Wood, Vincent Bourrier, Leonardo dos Santos, Christopher Johns-Krull, George W. King, Jeffrey L. Linsky, Sarah Peacock
Figure caption: The fractional uncertainty of intrinsic EUV flux post-ISM attenuation correction is shown as a function of the log10[N(H I)/cm−2] value and uncertainty on that value at nine discrete wavelengths between 100 and 900 Å. Bound–free (continuum) absorption from interstellar H I, He I, and He II dominates at these specific wavelengths. We have included uncertainty on the He abundance (0.08 ± 0.02) and the upper limit on the He ionization (<0.60) from J. Dupuis et al. (1995) in the simulations.
Paper: Toward a 2D H I Map of the Local Interstellar Medium
Authors: Allison Youngblood, Kevin France, Tommi Koskinen, James Paul Mason, Seth Redfield, Brian E. Wood, Vincent Bourrier, Leonardo dos Santos, Christopher Johns-Krull, George W. King, Jeffrey L. Linsky, Sarah Peacock
Figure caption: The fractional uncertainty of intrinsic Lyα flux post-ISM attenuation correction is shown as a function of the log10[N(H I)/cm−2] value and uncertainty on that value at six discrete wavelengths across the H I Lyα line. Near the line center (1215.67 Å or 0 km s−1), the ISM transmission is 0% regardless of the N(H I) value, so the fractional uncertainty is undefined. We have included uncertainty in the D I abundance (D/H = 1.56 ± 0.04 × 10−5) and Doppler broadening parameter for H I (b = 10.8 ± 1.0 km s−1) in the simulations.
Paper: Toward a 2D H I Map of the Local Interstellar Medium
Authors: Allison Youngblood, Kevin France, Tommi Koskinen, James Paul Mason, Seth Redfield, Brian E. Wood, Vincent Bourrier, Leonardo dos Santos, Christopher Johns-Krull, George W. King, Jeffrey L. Linsky, Sarah Peacock
Figure caption: Reconstructions following the methodology of V. Bourrier et al. (2017, 2018b, 2020) are shown for four targets included in this work. The black histograms with error bars show the STIS/G140M data, and the regions marked by the dashed green vertical lines were excluded from the fit due to airglow contamination. The solid green lines show the reconstructed intrinsic stellar profile, and the dotted black lines show the transmission of the ISM, where the top of the axis corresponds to 100% transmission and the bottom to 0% transmission. The solid blue lines show the stellar profile after absorption by the ISM, and the red lines show its convolution with the instrument line-spread function.