adsabs/AstroCLIMB huggingface dataset:
Paper: Improving H2RG Performance in SPHEREx Brassboard Model
Authors: Chi H. Nguyen, Phillip Korngut, C. Darren Dowell, James Bock, Jill Burnham, Samuel Condon, Walter Cook, Grigory Heaton, Howard Hui, Branislav Kecman, Hiromasa Miyasaka, Kenneth Manatt, Hien T. Nguyen, Stephen Padin, Marco Viero
Figure caption: (a) Photocurrents of rows 5–20 (Y coordinates = 5–20 in Figure 6) affected by the MUX glow (“MUX pixels”); rows 2024–2044 well outside of the MUX glow zones (“non-MUX”), which measure only the dark current; and the reference pixels. (b) The rms slope noise of the three populations (as calculated in Section 4.5). VBIASGATE >2.36 V pushes the electronics to its dynamical limit and degrades the detector performance, reflected in the fast rise in (b), so we only operate in the 2.30–2.36 V range (blue shaded zone).
Paper: Improving H2RG Performance in SPHEREx Brassboard Model
Authors: Chi H. Nguyen, Phillip Korngut, C. Darren Dowell, James Bock, Jill Burnham, Samuel Condon, Walter Cook, Grigory Heaton, Howard Hui, Branislav Kecman, Hiromasa Miyasaka, Kenneth Manatt, Hien T. Nguyen, Stephen Padin, Marco Viero
Figure caption: Noise powers as functions of Nvisit at (a) k < 0.03, (b) 0.03 ≤ k < 0.13, and (c) k ≥ 1. We see significant noise reduction on large scales in (a) and (b) up to Nvisit = 4; however, further samplings do not offer as significant reduction. The channel filtering offers the most noise reduction on large scales. Meanwhile, the pixel-to-pixel noises in (c) increase with higher Nvisit in all three corrections.
Paper: Improving H2RG Performance in SPHEREx Brassboard Model
Authors: Chi H. Nguyen, Phillip Korngut, C. Darren Dowell, James Bock, Jill Burnham, Samuel Condon, Walter Cook, Grigory Heaton, Howard Hui, Branislav Kecman, Hiromasa Miyasaka, Kenneth Manatt, Hien T. Nguyen, Stephen Padin, Marco Viero
Figure caption: High-level summary of the image construction steps. The phantom correction is unique to our application of the VIDEO8 drift monitoring. Additionally, to make the reference pixels a better analogy to the optical pixels, here we apply a multiplicative correction α to the reference pixels before subtraction (middle step in the blue box; Section 4.2).
Paper: Improving H2RG Performance in SPHEREx Brassboard Model
Authors: Chi H. Nguyen, Phillip Korngut, C. Darren Dowell, James Bock, Jill Burnham, Samuel Condon, Walter Cook, Grigory Heaton, Howard Hui, Branislav Kecman, Hiromasa Miyasaka, Kenneth Manatt, Hien T. Nguyen, Stephen Padin, Marco Viero
Figure caption: The 1D noise spectra of all Nvisit. Multiple samplings of the reference pixels improve the large-scale noise, but the improvement is not as pronounced at Nvisit > > 4, and the largest-scale noises still exceed the photon noise level (blue dashed line) unless the channel filtering is used.
Paper: Improving H2RG Performance in SPHEREx Brassboard Model
Authors: Chi H. Nguyen, Phillip Korngut, C. Darren Dowell, James Bock, Jill Burnham, Samuel Condon, Walter Cook, Grigory Heaton, Howard Hui, Branislav Kecman, Hiromasa Miyasaka, Kenneth Manatt, Hien T. Nguyen, Stephen Padin, Marco Viero
Figure caption: The time series of a single reference pixel in an exposure at SPHEREx flight cadence, mean subtracted by the time-averaged count to highlight the fluctuations around zero (thin gray). When smoothed by a five-frame kernel (thick black) to suppress the white noise, the time series exhibits clear low-frequency nonrandom fluctuations.
Paper: Improving H2RG Performance in SPHEREx Brassboard Model
Authors: Chi H. Nguyen, Phillip Korngut, C. Darren Dowell, James Bock, Jill Burnham, Samuel Condon, Walter Cook, Grigory Heaton, Howard Hui, Branislav Kecman, Hiromasa Miyasaka, Kenneth Manatt, Hien T. Nguyen, Stephen Padin, Marco Viero
Figure caption: Example production of constructing a dark exposure. (a) Slope map that includes phantom and H2RG photocurrent. (b) The phantom-corrected photocurrent map where the Video8 drift is removed. (c) The reference-subtracted map where the channel offset is removed using the mean of reference pixels. A 4 pixel Gaussian kernel is applied to the plots to better illustrate the noise on large spatial scales.
Paper: Improving H2RG Performance in SPHEREx Brassboard Model
Authors: Chi H. Nguyen, Phillip Korngut, C. Darren Dowell, James Bock, Jill Burnham, Samuel Condon, Walter Cook, Grigory Heaton, Howard Hui, Branislav Kecman, Hiromasa Miyasaka, Kenneth Manatt, Hien T. Nguyen, Stephen Padin, Marco Viero
Figure caption: The 2D power spectra of the noise maps using (a) reference subtraction as is and (b) channel filtering. By spatially smoothing the data in the x-direction, the latter removes the power concentrated on kx ≤ 0.05 modes.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Comparison between MicrolensingMetric results for several distinct iterations of the Rubin baseline strategy. The colors show the fractional improvement relative to baseline_v2.0_10yrs, where blue means that the metric has performed better relative to the baseline metric and red means that it has performed worse. On the x-axis are each of the OpSims, where 10yrs means that it was simulated for a 10 yr LSST survey. On the y-axis are each of the metrics for a t E range compared to their values for baseline_v2.0_10yrs. Shorter events (smaller t E) correspond to less massive objects such as brown dwarfs and low-mass stars, whereas longer events (larger t E) can correspond to black holes. The y-axis groups each set of metrics, and each line is a different t E range. The black horizontal lines indicate the separate metrics. “σ  tE /t E < 0.1'' refers to the Fisher Metric, “>10 pts” refers to the Npts Metric, and “Detected” refers to the Discovery Metric. For example, “σ  tE /t E < 0.1 t E = [30, 60] days” refers to the fraction of the 10,000 events with 30 days ≤ t E ≤ 60 days simulated as described in Section 2.3 with ﹩\tfrac{{\sigma }_{{t}_{{\rm{E}}}}}{{t}_{{\rm{E}}}}\lt 0.1﹩ as calculated by the Fisher information matrix. All of the current baselines show a ≳50% improvement over the retro baseline.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Same as Figure 5, but for the vary_gp, plane_priority, pencil, and galplane_priority families. The colors show the fractional improvement relative to baseline_v2.0_10yrs. Black vertical lines indicate separate OpSim families (summarized in Table 2), and black horizontal lines indicate separate metrics. Covering regions of lower stellar density and/or high extinction (areas of priority less than 0.4 as defined in R. A. Street et al. 2023b) leads to significant decrease in microlensing characterization efficiency. The pbf strategies do not include pencil beams selected in R. A. Street et al. (2023b) of scientific interest, whereas the pbt strategies include them. While the number of detected and characterized microlensing events does not significantly differ between them, since the pencil beams were specifically chosen to optimize our ability to probe the Galaxy, the strategy is preferable. The size of the pencil beams does not appear to significantly affect microlensing efficiency.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Microlensing parallax (Equation (7)) vs. Einstein crossing time (Equation (2)) for microlensing events simulated using PopSyCLE (C. Y. Lam & J. R. Lu 2020). Blue circles are stars, orange triangles are white dwarfs, green stars are neutron stars, and red squares are black holes. The ranges of t E and π E are cropped to match Figures 12–15. As shown in Equation (8), more massive lenses tend to be toward the lower right corner of this plot.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Flowchart of the MicrolensingMetric functionality. Either the user can input a t E range and generate microlensing events with a function known as a “Slicer,” or the user can input the events. The user can then choose to use the Discovery Metric, Npts Metric, or Fisher Metric. The Discovery Metric, by default, finds the fraction of events with N points on the rising side with at least a 3σ difference from baseline. The user can select detect = True to find at least N points on both the rising and falling side or alert = True to require the N points on the rising side to be a certain number of days before the peak. In this paper, we only explore the default mode of the Discovery Metric. The Npts Metric returns the number of points within t 0 ± t E with SNR >3σ, and the Fisher Metric returns the fraction of events with a fractional t E uncertainty <0.1.
Paper: Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time
Authors: Natasha S. Abrams, Markus P. G. Hundertmark, Somayeh Khakpash, Rachel A. Street, R. Lynne Jones, Jessica R. Lu, Etienne Bachelet, Yiannis Tsapras, Marc Moniez, Tristan Blaineau, Rosanne Di Stefano, Martin Makler, Anibal Varela, Markus Rabus
Figure caption: Example plot of a characterizable event with t E = 161 days, π E = 0.21, u 0 = 1.5, and ϕ = 0.79. It was simulated in a Galactic disk patch (R.A. = 288.°34, decl. = 9.°66) with baseline_v3.0_10yrs. Details of the simulation are described in Section 2.4. The parallax is characterized with a relative uncertainty of ﹩{\sigma }_{{\pi }_{{\rm{E}}}}/{\pi }_{{\rm{E}}}=0.06﹩, and the Einstein time is characterized with ﹩{\sigma }_{{t}_{{\rm{E}}}}/{t}_{{\rm{E}}}=0.06﹩. As is standard for achromatic microlensing events, all light curves are aligned and rescaled to the best data set. In this case, the r band serves as the reference baseline.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Frequency-spacing corrections for RC stars using the Garstec+Mosser (top left), Garstec+White (middle left), and Sharma+White (lower left) models and weights. Differences between Garstec+Mosser and Garstec+White (top right) measure the impact of the assigned weighting scheme. Differences between Garstec+White and Sharma+White measure the impact of the models used. For a minority of stars, the true ﹩{\rm{log}}g﹩ range of the sample did not correspond to the range in the model grid, which is responsible for some of the structures seen in the BeSPP results.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Our four cohorts—Gold (top left), Silver (top right), Detections (bottom left), and Nondetections (bottom right)—illustrated in 3D mesh plots as a function of ﹩{\rm{log}}g﹩ and spectroscopic Teff. We use seismic ﹩{\rm{log}}g﹩ for all categories except Nondetections, for which we use spectroscopic ﹩{\rm{log}}g﹩. The horizontal lines denote the approximate boundaries where we report masses and radii (between ﹩{\rm{log}}g﹩ of 1 and 3.3). Bin sizes of 40 K in Teff and 0.02 dex in ﹩{\rm{log}}g﹩ reflect typical measurement uncertainties. The vertical scale for the Gold bin is higher than for the other panels. The large majority of lower RGB and RC stars are robustly detected. In the detected groups, we also note the number of stars with detections that are outside the domain where we provide masses, ages, and radii. In total, we have 12,448 targets with full data, 1634 with partial data, and 1423 without seismic data. Background sources (129) and stars without valid spectroscopic data (174) are not shown.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Frequency-spacing corrections for RGB stars using the Garstec+Mosser (top left), Garstec+White (middle left), and Sharma+White (lower left) models and weights. Differences between Garstec+Mosser and Garstec+White (top right) measure the impact of the assigned weighting scheme. Differences between Garstec+White and Sharma+White measure the impact of the models used.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: The abundance distribution of the APOKASC-3 sample in the [α/Fe]–[Fe/H] plane. The red line is the criterion that we use to distinguish high [α/Fe] from low [α/Fe] ones. For plotting purposes later in the catalog, we use a slight modification of the J. D. Roberts et al. (2024) criterion for distinguishing the two populations. A star was classified as α-rich if [α/Fe] was above (0.08–0.15[Fe/H]) in the range −0.4 < [Fe/H] < +0.2; a threshold of +0.14 was assigned for [Fe/H] below −0.4; and a threshold of +0.05 was used for [Fe/H] above +0.2. Our criterion differs from the J. D. Roberts et al. (2024) one in that we use [α/Fe] and they used [Mg/Fe], including a slight zero-point shift.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Our four cohorts—Gold (dark yellow, circles), Silver (light gray, triangles), Detections (dark gray, squares), and Nondetections (orange, diamonds)—illustrated as a function of spectroscopic ﹩{\nu }_{{\rm{\max }}}﹩ for stars with <3 quarters of data (left) and for those with 3–18 quarters (right). Absolute numbers are in the top panels, and fractions in the bottom panels. The large majority of stars with good data are detected in our core domain of 1–220 μHz, while recovery is much more difficult for shorter time series.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Temperature offset, as defined in M. Vrard et al. (2024), relative to the mean RGB locus as a function of asteroseismic surface gravity for our upper RGB sample. The RC stars are shown in blue, RGB stars are red, and AGB stars are yellow. A 1 solar mass, solar metallicity MIST AGB track is shown for reference as a yellow line.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: The full APOKASC-3 evolved star sample. The histogram illustrates the number of targets, as a function of metallicity, in 0.05 dex ﹩{\rm{log}}g﹩ bins (right).
Paper: The Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX) Active Galactic Nuclei Catalog: The Fourth Data Release
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Matt J. Jarvis, Daniel J. Farrow, Steven L. Finkelstein, Óscar A. Chávez Ortiz
Figure caption: The redshift distributions of the HETDEX HDR4 AGN catalog. The blue histogram is for the full 15,940 AGN set. The orange histogram excludes the sIBL AGN candidates (agn_flag = 0, column 7 in Table 2). The green histogram further excludes the AGN with estimated redshifts only (zflag = 0, column 6 in Table 2). The gray histogram is the scaled redshift distributions of the SDSS DR16Q sample to generally match the number of HETDEX AGN at z ∼ 1.5.
Paper: The Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX) Active Galactic Nuclei Catalog: The Fourth Data Release
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Matt J. Jarvis, Daniel J. Farrow, Steven L. Finkelstein, Óscar A. Chávez Ortiz
Figure caption: Similar format as Figure 5 but for the HETDEX g-band magnitudes. While g-band magnitudes are plotted as computed, the 5σ depth of HETDEX is roughly 25, marked by the shaded area.
Paper: The Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX) Active Galactic Nuclei Catalog: The Fourth Data Release
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Matt J. Jarvis, Daniel J. Farrow, Steven L. Finkelstein, Óscar A. Chávez Ortiz
Figure caption: Example HETDEX AGN spectra covering the redshift range of the catalog. The resolution of the spectra is 2 Å.
Paper: The DiskMass Survey. XI. Disk Geometries and Star Formation Surface Densities from Ionized Gas Kinematics and Line Intensities for the Full Hα Sample
Authors: Robert A. Swaters, David R. Andersen, Matthew A. Bershady, Thomas P. K. Martinsson, Paul Scholz, Marc A.W. Verheijen, Kyle B. Westfall
Figure caption: Flux zero-point in mag arcsec−2 (Johnson R-band) corresponding to 1 DN pixel−1 fiber−1 for DiskMass Hα observations made over 4 yr using SparsePak and the Bench spectrograph on the WIYN 3.5 m telescope. The inset histogram gives random errors on individual calibration measurements, which is 5 times lower than the standard deviation between all objects and measurements (dashed lines). Several significant outliers are marked by their UGC number.
Paper: The DiskMass Survey. XI. Disk Geometries and Star Formation Surface Densities from Ionized Gas Kinematics and Line Intensities for the Full Hα Sample
Authors: Robert A. Swaters, David R. Andersen, Matthew A. Bershady, Thomas P. K. Martinsson, Paul Scholz, Marc A.W. Verheijen, Kyle B. Westfall
Figure caption: Resulting Hα emission lines after sky subtraction (top panels) and the subtracted sky (bottom panels) when taking the average of sky fibers (left panels) or using a progressive clipping method (right panels). Though progressive clipping does result in more uniform noise in the sky-subtracted image, some emission may be included in the calculated sky, which can impact the derived centroids. This example for UGC 11318 was chosen because the effect is stronger due to the emission lines all being at similar wavelengths.