adsabs/AstroCLIMB huggingface dataset:
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: ξ (location), ω (scale), and α (skewness) parameters in AGAMA for Zv, following its representation as a skewed-normal distribution (Equation (7)), for a 1015 M⊙ cluster at redshift z = 0.01, inferred for 1000 different viewing angles in the innermost bin. Other bin, redshift, and mass choices follow similar trends, with each parameter following a linear scaling in ﹩{\mathrm{log}}(N)﹩ space.
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: Agreement between weak lensing and the caustic masses for the H20 sample. There is a very large observed bias and poor correlation (see Table 4), despite the fact that we should see better agreement between caustics and weak lensing, as discussed in Section 1.
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: Fractional differences between the suppression values of a grid of velocity gap and binning choices for the shifting-gapper (D. Gifford & C. J. Miller 2013), and a fixed fiducial measurement, analogous to A. Rodriguez et al. (2024). There is an obvious trend toward increasing stability of the parameter choice, which is used for robust identification of interlopers.
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: The normalized distributions of the suppression (Zv) in AGAMA for an N = 50 (top panel) and N = 1000 (bottom panel) for a 1015 M⊙ cluster at redshift z = 0.01, inferred for 1000 different viewing angles in the innermost bin. The black lines correspond to fits to the distributions using the skewness, location, and scale (A. Azzalini & A. Capitanio 2009). The poorly sampled system exhibits high suppression values and a long tail.
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: Same as Figure 8, except for the two full observational samples. Both individual samples have improved biases and correlations over Figure 7. The agreement between the samples indicates sample selection is not a significant systematic (see Section 4.3).
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Distribution of SED χ2 values as a function of base density for HDUST models at two distances (703 pc and 888 pc) and two density slope parameters (n = 3.0 and n = 3.5). Each panel shows the same data colored by different free parameters: companion’s effective temperature (left panel), companion’s radius (central panel), and interstellar extinction E(B − V; right panel). Diamonds represent models at 703 pc, circles represent models at 888 pc. Larger symbols correspond to n = 3.0, smaller symbols to n = 3.5. Gray lines connect models with identical distance and slope parameters to highlight density-dependent trends. Lower χ2 values indicate better fits to the observed SED.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Top panels: comparison of HDUST-generated most-probable solution model (purple solid line) with the average observed Hα (left panel) and Hβ (right panel) line profiles (black solid line). The model includes contributions from the Be star and its disk (yellow dashed line) and the companion (green dashed line). Bottom panels: same, but companion’s flux assumed to be flat. For each panel, we report the EWs for comparison: top left (Hα): EWobserved = −9.47 Å, EWmodel = −2.61 Å; top right (Hβ): EWobserved = 1.10 Å, EWmodel = 2.39 Å; bottom left (Hα): EWobserved = −9.47 Å, EWmodel = − 4.51 Å; bottom right (Hβ): EWobserved = 1.10 Å, EWmodel = 0.31 Å.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: H-R diagrams with evolutionary tracks of the mass donor from two BPASS binary evolution models. The location of HR 698 is given by the red “x” and star symbols for the Be and bloated component, respectively. The two BPASS models of Table 6 are shown in the top and bottom rows, respectively. Left to right, the tracks are colored by the mass donor’s radius, hydrogen abundance, and helium abundance.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Top panel: the total modeled SED (purple solid line) is the sum of the Be star and its disk (yellow solid line) and companion’s (green dashed line) contributions, both generated with HDUST. Observational data is shown in black. The yellow dashed line represents flux contribution from the disk. Bottom panel: residuals distribution across wavelengths.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Corner plots of the MCMC posteriors for the model with disk base density ρ0 = 2.5 × 10−12 g cm−3.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Comparison of HD 698’s components (magenta stars) on H-R diagram with known Be+sdO binaries (green circles; D. R. Gies et al. 1998; G. J. Peters et al. 2008, 2013; D. Mourard et al. 2015; G. J. Peters et al. 2016; L. Wang et al. 2017; S. D. Chojnowski et al. 2018; L. Wang et al. 2021; R. Klement et al. 2024), Be+sdB binaries (orange circles) (R. Klement et al. 2022; T. H. de Amorim et al. 2025), and three example Be+bloated O/B binaries from Table 5 (blue circles).
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: EW comparison of HDUST-generated absorption lines with the observed spectrum. The black dashed line indicates a perfect fit.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Corner plots of the MCMC posteriors for the model with disk base density ρ0 = 7.5 × 10−12 g cm−3.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Corner plots of the MCMC posteriors for the model with disk base density ρ0 = 5.0 × 10−12 g cm−3.
Paper: Comparing Inside-out and Outside-in Quenching Modes in MaNGA Observation and MaNGIA Simulation
Authors: Hung-Yu Jian, Lihwai Lin, Connor Bottrell, Bau-Ching Hsieh, Carlos López-Cobá, Zi-Hua Ho, Shuai Feng, Shiyin Shen
Figure caption: The fractions of galaxies classified as undergoing inside-out (left column) and outside-in (right column) quenching, plotted as a function of galaxy type (central/satellite), stellar mass (M*), and halo mass (Mh) for the MaNGA (left panels) and MaNGIA (right panels) samples. Central galaxies with log10(M*/M⊙) > 10.5 are indicated by solid red lines, while satellite galaxies are shown with yellow (log10(M*/M⊙) = 9–9.75), green (log10(M*/M⊙) = 9.75–10.5), and blue (log10(M*/M⊙) > 10.5) lines. The MaNGA results demonstrate a dominant inside-out quenching mode in massive galaxies and a dominant outside-in mode in less massive galaxies. A similar overall trend is observed in the MaNGIA data, although the distinction is less pronounced.
Paper: Comparing Inside-out and Outside-in Quenching Modes in MaNGA Observation and MaNGIA Simulation
Authors: Hung-Yu Jian, Lihwai Lin, Connor Bottrell, Bau-Ching Hsieh, Carlos López-Cobá, Zi-Hua Ho, Shuai Feng, Shiyin Shen
Figure caption: The global (left column) and resolved (right column) star-forming main sequence for the MaNGA (upper left panel, solid blue line) and MaNGIA (upper right panel, dashed blue line) samples. The lower panels display the median SFR as a function of M* (left) and the median ΣSFR as a function of Σ* (right), with error bars representing the standard deviation. The star formation rate in MaNGA is estimated from Hα flux. Global SFR and M* are derived by coadding the surface densities within 1.5 effective radii. The green (or white) solid line indicates the separation between star-forming and quiescent populations based on log10(sSFR) = –11 (left column) or log10(ΣsSFR) = −11 (right column). A clear correlation between the two samples is observed for the star-forming main sequence in both global and resolved regimes.
Paper: Comparing Inside-out and Outside-in Quenching Modes in MaNGA Observation and MaNGIA Simulation
Authors: Hung-Yu Jian, Lihwai Lin, Connor Bottrell, Bau-Ching Hsieh, Carlos López-Cobá, Zi-Hua Ho, Shuai Feng, Shiyin Shen
Figure caption: Illustration of a galaxy classified as inside-out quenched based on the mean radial component of the gradient of the specific star formation rate surface density, 〈∇rΣsSFR〉. The upper left panel highlights spaxels exhibiting color-coded positive radial sSFR gradients, while the upper right panel shows those with color-coded negative gradients. The bottom left panel presents the radial components of the ΣsSFR gradient for all spaxels located within 1.5 effective radii (Re). Across these three gradient maps, arrow length scales with gradient magnitude, and arrow direction denotes radial (inward or outward) orientation. The bottom right panel provides a map of ΣsSFR on a logarithmic scale for individual spaxels, overlaid with three red ellipses indicating 0.5, 1.0, and 1.5 Re, respectively.
Paper: Comparing Inside-out and Outside-in Quenching Modes in MaNGA Observation and MaNGIA Simulation
Authors: Hung-Yu Jian, Lihwai Lin, Connor Bottrell, Bau-Ching Hsieh, Carlos López-Cobá, Zi-Hua Ho, Shuai Feng, Shiyin Shen
Figure caption: The distribution of central and satellite galaxies from the MaNGA (upper panel) and MaNGIA (lower panel) samples as a function of host halo mass (Mh) and stellar mass (M*), with redshift indicated by the color scale. The yellow grid delineates the discrete bins used for subsequent analysis, and the number of galaxies within each bin is overlaid in red. We note that the vertical striations in the data for MaNGA and MaNGIA satellite galaxies arise from satellites residing in halos with the same host halo masses.
Paper: Comparing Inside-out and Outside-in Quenching Modes in MaNGA Observation and MaNGIA Simulation
Authors: Hung-Yu Jian, Lihwai Lin, Connor Bottrell, Bau-Ching Hsieh, Carlos López-Cobá, Zi-Hua Ho, Shuai Feng, Shiyin Shen
Figure caption: The median stellar mass surface density (Σ*) as a function of normalized radius for galaxies in the MaNGA (solid lines) and MaNGIA (dashed lines) samples, divided into four distinct stellar mass (M*) bins: log10(M*/M⊙) = [8, 9] (yellow), [9, 10] (red), [10, 11] (green), and >11 (blue). The error bars represent the standard deviation of Σ* within each radial bin for the respective mass range. A generally good agreement is observed between the radial Σ* profiles of the two samples across all considered stellar mass bins.
Paper: Comparing Inside-out and Outside-in Quenching Modes in MaNGA Observation and MaNGIA Simulation
Authors: Hung-Yu Jian, Lihwai Lin, Connor Bottrell, Bau-Ching Hsieh, Carlos López-Cobá, Zi-Hua Ho, Shuai Feng, Shiyin Shen
Figure caption: Distributions of MaNGA (left) and MaNGIA (right) galaxies on the quiescence (Fq) versus quenching concentration (Cq) plane. The plots are color-coded by stellar mass (M*). Galaxies are classified as inside-out quenched (green) or outside-in quenched (purple) based on their specific location within this parameter space.
Paper: Comparing Inside-out and Outside-in Quenching Modes in MaNGA Observation and MaNGIA Simulation
Authors: Hung-Yu Jian, Lihwai Lin, Connor Bottrell, Bau-Ching Hsieh, Carlos López-Cobá, Zi-Hua Ho, Shuai Feng, Shiyin Shen
Figure caption: Stellar mass histograms comparing the original total galaxy distributions (left panel) of MaNGA and MaNGIA with their matched samples (right panel).
Paper: DESI Spectroscopy of HETDEX Emission-line Candidates. I. Line Discrimination Validation
Authors: Martin Landriau, Erin Mentuch Cooper, Dustin Davis, Karl Gebhardt, Robin Ciardullo, Éric Armengaud, Arjun Dey, Anand Raichoor, David J. Schlegel, Michael Wilson, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, L. Le Guillou, Michael E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, I. Pérez-Ràfols, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou, Daniel J. Farrow, Gary J. Hill, Donghui Jeong, Chenxu Liu, Shun Saito, Donald P. Schneider
Figure caption: The top panel shows the distribution of emission-line detection S/N for HETDEX targets. The gray histogram indicates the range in the input target sample, while the blue histogram shows the recovered galaxies with VI_quality ≥ 3. The cumulative recovery fraction as a function of S/N is shown in dashed gray for the full sample and in dashed black where some cuts are applied. Only well-positioned sources with emission lines λ > 3800 Å, and those that have not been excluded from later HETDEX catalogs, are included in this sample (i.e., we only include those emission lines with DEX_FLAG == 1 and WAVE_HETDEX >3800.0). Sources at low S/N are missed owing to astrometric uncertainties for low-S/N sources and possible false positives. The bottom panel presents the distribution in gHETDEX magnitudes of the input and recovered sample in gray and blue, respectively.
Paper: DESI Spectroscopy of HETDEX Emission-line Candidates. I. Line Discrimination Validation
Authors: Martin Landriau, Erin Mentuch Cooper, Dustin Davis, Karl Gebhardt, Robin Ciardullo, Éric Armengaud, Arjun Dey, Anand Raichoor, David J. Schlegel, Michael Wilson, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, L. Le Guillou, Michael E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, I. Pérez-Ràfols, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou, Daniel J. Farrow, Gary J. Hill, Donghui Jeong, Chenxu Liu, Shun Saito, Donald P. Schneider
Figure caption: The results of our comparison of ELiXer classifications of HETDEX spectra with the high-confidence, visually vetted DESI spectra. The y-axis gives the percent contamination of the HETDEX LAE sample by misidentified [O II] galaxies, while the percentage of LAEs recovered by the classifier is on the x-axis. The labeled points show the corresponding P(Lyα) threshold used to configure the ELiXer classifier. The red horizontal dashed line represents the requirements of the HETDEX survey (K. Gebhardt et al. 2021), though higher contamination rates may be acceptable with the use of additional decontamination methodologies (D. J. Farrow et al. 2021). Despite differences in the redshift and magnitude distributions with the Spectroscopic-z Assessment Sample in D. Davis et al. (2023), the curve is very similar.
Paper: DESI Spectroscopy of HETDEX Emission-line Candidates. I. Line Discrimination Validation
Authors: Martin Landriau, Erin Mentuch Cooper, Dustin Davis, Karl Gebhardt, Robin Ciardullo, Éric Armengaud, Arjun Dey, Anand Raichoor, David J. Schlegel, Michael Wilson, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, L. Le Guillou, Michael E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, I. Pérez-Ràfols, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou, Daniel J. Farrow, Gary J. Hill, Donghui Jeong, Chenxu Liu, Shun Saito, Donald P. Schneider
Figure caption: Examples of fitted Lyα lines for DESI on the left and HETDEX on the right. Each row represents a single LAE. The Lyα flux values in the legends are reported in units of 10−17 erg s−1 cm−2 Å−1. In the bottom example, the line is double peaked; as a result, the fitted line width is higher for HETDEX than for the DESI line fit, which only fits the brightest component of the line.
Paper: DESI Spectroscopy of HETDEX Emission-line Candidates. I. Line Discrimination Validation
Authors: Martin Landriau, Erin Mentuch Cooper, Dustin Davis, Karl Gebhardt, Robin Ciardullo, Éric Armengaud, Arjun Dey, Anand Raichoor, David J. Schlegel, Michael Wilson, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, L. Le Guillou, Michael E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, I. Pérez-Ràfols, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou, Daniel J. Farrow, Gary J. Hill, Donghui Jeong, Chenxu Liu, Shun Saito, Donald P. Schneider
Figure caption: Comparison of redshifts obtained from visual inspection, VI_Z, of DESI spectra (x-axis) and those derived from HETDEX data (y-axis) using ELiXer. The plot assumes a P(Lyα) = 0.5 threshold for the HETDEX line classifications. As discussed in Section 4, this value leads to a 1.15% contamination of the LAE sample by [O II] galaxies and a loss of 5.6% true LAEs from the HETDEX sample.
Paper: DESI Spectroscopy of HETDEX Emission-line Candidates. I. Line Discrimination Validation
Authors: Martin Landriau, Erin Mentuch Cooper, Dustin Davis, Karl Gebhardt, Robin Ciardullo, Éric Armengaud, Arjun Dey, Anand Raichoor, David J. Schlegel, Michael Wilson, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, L. Le Guillou, Michael E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, I. Pérez-Ràfols, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou, Daniel J. Farrow, Gary J. Hill, Donghui Jeong, Chenxu Liu, Shun Saito, Donald P. Schneider
Figure caption: Example DESI spectra of a faint [O II] galaxy at z = 0.318 (top) and an LAE at z = 2.984 (bottom) confirmed by visual inspection.
Paper: DESI Spectroscopy of HETDEX Emission-line Candidates. I. Line Discrimination Validation
Authors: Martin Landriau, Erin Mentuch Cooper, Dustin Davis, Karl Gebhardt, Robin Ciardullo, Éric Armengaud, Arjun Dey, Anand Raichoor, David J. Schlegel, Michael Wilson, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, L. Le Guillou, Michael E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, I. Pérez-Ràfols, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou, Daniel J. Farrow, Gary J. Hill, Donghui Jeong, Chenxu Liu, Shun Saito, Donald P. Schneider
Figure caption: Parent and assigned target distributions for the two pointings. The numbers 80869 and 80870 refer to the DESI tile ID, which is unique for the combination of pointing and fiber assignments. Gaps in the assigned target distribution where there were available targets in the parent sample are due to fibers being assigned to other secondary target programs or small regions of the focal plane with nonworking fiber-positioning robots during that period.
Paper: DESI Spectroscopy of HETDEX Emission-line Candidates. I. Line Discrimination Validation
Authors: Martin Landriau, Erin Mentuch Cooper, Dustin Davis, Karl Gebhardt, Robin Ciardullo, Éric Armengaud, Arjun Dey, Anand Raichoor, David J. Schlegel, Michael Wilson, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, L. Le Guillou, Michael E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, I. Pérez-Ràfols, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou, Daniel J. Farrow, Gary J. Hill, Donghui Jeong, Chenxu Liu, Shun Saito, Donald P. Schneider
Figure caption: HETDEX main (aka “spring”) field outlined in blue, with completion status as indicated by orange tiles as of 2021 January, when the target list for the sample was selected (the gray tiles were planned but yet to be observed). The two circles show the positions of the two DESI tiles chosen for the follow-up.