adsabs/AstroCLIMB huggingface dataset:
Paper: Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass
Authors: Andrew W. Mayo, Courtney D. Dressing, Andrew Vanderburg, Charles D. Fortenbach, Florian Lienhard, Luca Malavolta, Annelies Mortier, Alejandro Núñez, Tyler Richey-Yowell, Emma V. Turtelboom, Aldo S. Bonomo, David W. Latham, Mercedes López-Morales, Evgenya Shkolnik, Alessandro Sozzetti, Marcel A. Agüeros, Luca Borsato, David Charbonneau, Rosario Cosentino, Stephanie T. Douglas, Xavier Dumusque, Adriano Ghedina, Rose Gibson, Valentina Granata, Avet Harutyunyan, R. D. Haywood, Gaia Lacedelli, Vania Lorenzi, Antonio Magazzù, A. F. Martinez Fiorenzano, Giuseppina Micela, Emilio Molinari, Marco Montalto, Domenico Nardiello, Valerio Nascimbeni, Isabella Pagano, Giampaolo Piotto, Lorenzo Pino, Ennio Poretti, Gaetano Scandariato, Stephane Udry, Lars A. Buchhave
Figure caption: Top: mass–radius diagram of transiting planets with fractional mass and radius uncertainties less than 50%. K2-136b, c, and d are plotted in dark orange, with mass uncertainties on K2-136b and d as 68% and 95% upper limits denoted in light orange. Data collected from the NASA Exoplanet Archive (accessed 2023 Mar 22; NASA Exoplanet Science Institute 2020). Venus, Earth, Uranus, and Neptune are also labeled and plotted in blue for reference. Except for the K2-136 system, planets with larger fractional mass and radius uncertainties are fainter. Gray lines correspond to planetary compositions (from top to bottom) of 100% H2O, 50% H2O, 25% H2O, 100% MgSiO3, 50% MgSiO3 + 50% Fe, and 100% Fe, respectively (Zeng & Sasselov 2013; Zeng et al. 2016). Kepler-136c lies closest to the 100% H2O composition line, and is similar in mass to Uranus and Neptune although smaller and much more dense. Middle: the same sample plotted in mass vs. planet density, with the same solar system references and composition lines (order inverted from top panel). Bottom: the same sample plotted in planet insolation flux vs. planet density, with the color of all data points corresponding to planet mass (except for K2-136b and d, which only have mass upper limits and thus are plotted in light orange).
Paper: Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass
Authors: Andrew W. Mayo, Courtney D. Dressing, Andrew Vanderburg, Charles D. Fortenbach, Florian Lienhard, Luca Malavolta, Annelies Mortier, Alejandro Núñez, Tyler Richey-Yowell, Emma V. Turtelboom, Aldo S. Bonomo, David W. Latham, Mercedes López-Morales, Evgenya Shkolnik, Alessandro Sozzetti, Marcel A. Agüeros, Luca Borsato, David Charbonneau, Rosario Cosentino, Stephanie T. Douglas, Xavier Dumusque, Adriano Ghedina, Rose Gibson, Valentina Granata, Avet Harutyunyan, R. D. Haywood, Gaia Lacedelli, Vania Lorenzi, Antonio Magazzù, A. F. Martinez Fiorenzano, Giuseppina Micela, Emilio Molinari, Marco Montalto, Domenico Nardiello, Valerio Nascimbeni, Isabella Pagano, Giampaolo Piotto, Lorenzo Pino, Ennio Poretti, Gaetano Scandariato, Stephane Udry, Lars A. Buchhave
Figure caption: Left: Phased RV plots for all three K2-136 planets. For each subplot, we used our best-fit model parameters to remove stellar activity and the presence of the other two planets. In each subplot, blue data points (HARPS-N) and orange data points (ESPRESSO) are unbinned RV observations. The black line is the median fit and the gray region around that line is the 1σ confidence interval. Right: Posterior mass distribution plots for all three K2-136 planets. It is visually apparent that while there is a strong mass detection for K2-136c (R  p  = 3.00 ± 0.13 R ⊕), there is at best only a marginal detection for K2-136b (R  p  = 1.014 ± 0.050 R ⊕) and no evidence of a detection for K2-136d (R  p  = 1.565 ± 0.077 R ⊕). Therefore, we report only place upper limits on the masses of K2-136b and K2-136d (see Table 4).
Paper: Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass
Authors: Andrew W. Mayo, Courtney D. Dressing, Andrew Vanderburg, Charles D. Fortenbach, Florian Lienhard, Luca Malavolta, Annelies Mortier, Alejandro Núñez, Tyler Richey-Yowell, Emma V. Turtelboom, Aldo S. Bonomo, David W. Latham, Mercedes López-Morales, Evgenya Shkolnik, Alessandro Sozzetti, Marcel A. Agüeros, Luca Borsato, David Charbonneau, Rosario Cosentino, Stephanie T. Douglas, Xavier Dumusque, Adriano Ghedina, Rose Gibson, Valentina Granata, Avet Harutyunyan, R. D. Haywood, Gaia Lacedelli, Vania Lorenzi, Antonio Magazzù, A. F. Martinez Fiorenzano, Giuseppina Micela, Emilio Molinari, Marco Montalto, Domenico Nardiello, Valerio Nascimbeni, Isabella Pagano, Giampaolo Piotto, Lorenzo Pino, Ennio Poretti, Gaetano Scandariato, Stephane Udry, Lars A. Buchhave
Figure caption: Periodograms of RV, CCF FWHM, CCF BIS, and S  HK  for the K2-136 system. In the top panel is the window function (computed from observation times only). Each subplot has the periodogram of HARPS-N and ESPRESSO combined (black), HARPS-N alone (blue), and ESPRESSO alone (orange). The gray region corresponds to the 1σ confidence interval of the stellar rotation period (as determined from our model results); the three vertical, black lines correspond to the orbital periods of K2-136b, c, and d. Finally, the horizontal dashed lines refer to different false-alarm probabilities (for HARPS-N and ESPRESSO combined).
Paper: Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass
Authors: Andrew W. Mayo, Courtney D. Dressing, Andrew Vanderburg, Charles D. Fortenbach, Florian Lienhard, Luca Malavolta, Annelies Mortier, Alejandro Núñez, Tyler Richey-Yowell, Emma V. Turtelboom, Aldo S. Bonomo, David W. Latham, Mercedes López-Morales, Evgenya Shkolnik, Alessandro Sozzetti, Marcel A. Agüeros, Luca Borsato, David Charbonneau, Rosario Cosentino, Stephanie T. Douglas, Xavier Dumusque, Adriano Ghedina, Rose Gibson, Valentina Granata, Avet Harutyunyan, R. D. Haywood, Gaia Lacedelli, Vania Lorenzi, Antonio Magazzù, A. F. Martinez Fiorenzano, Giuseppina Micela, Emilio Molinari, Marco Montalto, Domenico Nardiello, Valerio Nascimbeni, Isabella Pagano, Giampaolo Piotto, Lorenzo Pino, Ennio Poretti, Gaetano Scandariato, Stephane Udry, Lars A. Buchhave
Figure caption: K2-136 observations and model fits for RVs (and fit residuals). In each panel, the blue points (HARPS-N) or orange points (ESPRESSO) are the observations while the black line and gray region are the model fit and 1σ confidence interval, respectively. The RVs have been mean-subtracted (corresponding to their respective instrument), and planet-induced reflex motion has been subtracted as well. RV errors have been inflated from their original values by adding the model-estimated RV jitter term in quadrature. Note the two time gaps between the first 88 HARPS-N observations, the 22 ESPRESSO observations, and the final 5 HARPS-N observations.
Paper: Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass
Authors: Andrew W. Mayo, Courtney D. Dressing, Andrew Vanderburg, Charles D. Fortenbach, Florian Lienhard, Luca Malavolta, Annelies Mortier, Alejandro Núñez, Tyler Richey-Yowell, Emma V. Turtelboom, Aldo S. Bonomo, David W. Latham, Mercedes López-Morales, Evgenya Shkolnik, Alessandro Sozzetti, Marcel A. Agüeros, Luca Borsato, David Charbonneau, Rosario Cosentino, Stephanie T. Douglas, Xavier Dumusque, Adriano Ghedina, Rose Gibson, Valentina Granata, Avet Harutyunyan, R. D. Haywood, Gaia Lacedelli, Vania Lorenzi, Antonio Magazzù, A. F. Martinez Fiorenzano, Giuseppina Micela, Emilio Molinari, Marco Montalto, Domenico Nardiello, Valerio Nascimbeni, Isabella Pagano, Giampaolo Piotto, Lorenzo Pino, Ennio Poretti, Gaetano Scandariato, Stephane Udry, Lars A. Buchhave
Figure caption: Transit plot of K2-136. The top and bottom subplots of the top plot are the raw and normalized K2 photometry vs. time from Campaign 13, respectively. In the top subplots of the bottom plot are the phase-folded light curves and transit model fits for K2-136b, c, and d. The gray points are the raw data. The best-fit transit model is the orange line, and binning is represented by the blue points. The bottom subplots of the bottom plot are the residuals after the best-fit model has been subtracted.
Paper: Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass
Authors: Andrew W. Mayo, Courtney D. Dressing, Andrew Vanderburg, Charles D. Fortenbach, Florian Lienhard, Luca Malavolta, Annelies Mortier, Alejandro Núñez, Tyler Richey-Yowell, Emma V. Turtelboom, Aldo S. Bonomo, David W. Latham, Mercedes López-Morales, Evgenya Shkolnik, Alessandro Sozzetti, Marcel A. Agüeros, Luca Borsato, David Charbonneau, Rosario Cosentino, Stephanie T. Douglas, Xavier Dumusque, Adriano Ghedina, Rose Gibson, Valentina Granata, Avet Harutyunyan, R. D. Haywood, Gaia Lacedelli, Vania Lorenzi, Antonio Magazzù, A. F. Martinez Fiorenzano, Giuseppina Micela, Emilio Molinari, Marco Montalto, Domenico Nardiello, Valerio Nascimbeni, Isabella Pagano, Giampaolo Piotto, Lorenzo Pino, Ennio Poretti, Gaetano Scandariato, Stephane Udry, Lars A. Buchhave
Figure caption: Mg II surface flux as a function of the stellar rotation period for K star Hyades members. The blue star represents K2-136, and the black points are the 13 other K star Hyades observed in a broader HST program (GO-15091, PI: Agüeros). The rotation periods are from Douglas et al. (2019) and have assumed errors of 10%, except for K2-136, which we determined to be ﹩{13.88}_{-0.18}^{+0.17}﹩ days in this work. K2-136 does not show any distinct chromospheric activity or unique rotation period compared to the rest of the sample.
Paper: COSMOS2020: Exploring the Dawn of Quenching for Massive Galaxies at 3 < z < 5 with a New Color-selection Method
Authors: Katriona M. L. Gould, Gabriel Brammer, Francesco Valentino, Katherine E. Whitaker, John. R. Weaver, Claudia del P. Lagos, Francesca Rizzo, Maximilien Franco, Bau-Ching Hsieh, Olivier Ilbert, Shuowen Jin, Georgios Magdis, Henry J. McCracken, Bahram Mobasher, Marko Shuntov, Charles L. Steinhardt, Victoria Strait, Sune Toft
Figure caption: Left: NUV − U, V − J colors of our massive (10.6 < log(M */M ⊙) < 12) galaxy sample at 3 < z < 5 (gray) and evolution tracks for an SSP with A  V  = 0 (blue line on the left of the figure) and A  V  = 1 (dark blue line) and Chabrier IMF aged to 1 Gyr. The dust vector representing the movement of a galaxy in this space by an attenuation of A  V  = 1 is shown by the arrow at the bottom right. Right: same but for UVJ with the quiescent box defined by Whitaker et al. (2012; defined as U − V > 0.8 × (V − J) + 0.7, U − V > 1.3 and V − J < 1.5).
Paper: COSMOS2020: Exploring the Dawn of Quenching for Massive Galaxies at 3 < z < 5 with a New Color-selection Method
Authors: Katriona M. L. Gould, Gabriel Brammer, Francesco Valentino, Katherine E. Whitaker, John. R. Weaver, Claudia del P. Lagos, Francesca Rizzo, Maximilien Franco, Bau-Ching Hsieh, Olivier Ilbert, Shuowen Jin, Georgios Magdis, Henry J. McCracken, Bahram Mobasher, Marko Shuntov, Charles L. Steinhardt, Victoria Strait, Sune Toft
Figure caption: Left: Δlog(SFR) (EAZY-PROSPECTOR) as a function of PROSPECTOR SFR for 8134 galaxies at 0.5 < z < 3.0 matched to our catalog with that of the 3D-HST survey in COSMOS. The median Δlog(SFR) is 0.07 dex (shown as red dashed line) and the scatter is 0.55 dex. The binned median offset and the associated 16th and 84th percentiles are shown as red points with error bars. Right: Δlog(M *) (EAZY-PROSPECTOR) as a function of PROSPECTOR stellar mass for the same sample. The median Δlog(M *) is 0.04 dex and the scatter is 0.21 dex. The binned mean offset and the associated 16th and 84th percentiles are shown as red points with error bars.
Paper: COSMOS2020: Exploring the Dawn of Quenching for Massive Galaxies at 3 < z < 5 with a New Color-selection Method
Authors: Katriona M. L. Gould, Gabriel Brammer, Francesco Valentino, Katherine E. Whitaker, John. R. Weaver, Claudia del P. Lagos, Francesca Rizzo, Maximilien Franco, Bau-Ching Hsieh, Olivier Ilbert, Shuowen Jin, Georgios Magdis, Henry J. McCracken, Bahram Mobasher, Marko Shuntov, Charles L. Steinhardt, Victoria Strait, Sune Toft
Figure caption: Photometric redshift vs. spectroscopic redshift for all galaxies at 0 < z < 5 in the combined UVISTA and HSC area with a K  s  S/N > 5. Red points are spectroscopically confirmed QGs at z > 2 from Schreiber et al. (2018), Stockmann et al. (2019), D’Eugenio et al. (2021), Forrest et al. (2020b), and Valentino et al. (2020).
Paper: Target Selection and Validation of DESI Emission Line Galaxies
Authors: A. Raichoor, J. Moustakas, Jeffrey A. Newman, T. Karim, S. Ahlen, Shadab Alam, S. Bailey, D. Brooks, K. Dawson, A. de la Macorra, A. de Mattia, A. Dey, Biprateep Dey, G. Dhungana, S. Eftekharzadeh, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. García-Bellido, E. Gaztañaga, S. Gontcho A Gontcho, J. Guy, K. Honscheid, M. Ishak, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, M. Manera, P. Martini, Aaron M. Meisner, Adam D. Myers, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. J. Ross, V. Ruhlmann-Kleider, C. G. Sabiu, E. F. Schlafly, D. Schlegel, Gregory Tarlé, B. A. Weaver, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Main ELG target selection cuts in the g − r vs. r − z diagram. The “ELG_LOP” and “ELG_VLO” selections are displayed as the solid black lines and the dashed red lines, respectively. The background symbols describe a g fib < 24.1 sample; the color-coding indicates the mean HSC/DR2 z phot measurements, and the transparency scales with the logarithm of the density. The thin black contour indicates the stellar locus. The tracks show the stellar evolutions of a highly star-forming galaxy (solid green line) and a moderately star-forming galaxy (dashed red line), observed at z spec 2.0, 1.6, 1.1, 0.6, and 0.1 (the square, downward triangle, circle, upward triangle, and star, respectively). See the text for more details.
Paper: Target Selection and Validation of DESI Emission Line Galaxies
Authors: A. Raichoor, J. Moustakas, Jeffrey A. Newman, T. Karim, S. Ahlen, Shadab Alam, S. Bailey, D. Brooks, K. Dawson, A. de la Macorra, A. de Mattia, A. Dey, Biprateep Dey, G. Dhungana, S. Eftekharzadeh, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. García-Bellido, E. Gaztañaga, S. Gontcho A Gontcho, J. Guy, K. Honscheid, M. Ishak, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, M. Manera, P. Martini, Aaron M. Meisner, Adam D. Myers, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. J. Ross, V. Ruhlmann-Kleider, C. G. Sabiu, E. F. Schlafly, D. Schlegel, Gregory Tarlé, B. A. Weaver, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: SV ELG target selection cuts in the g − r vs. r − z diagram (top) and (g − r) + 1.2 × (r − z) vs. g fib diagram (bottom). The ELG_LOP and ELG_VLO selections are displayed as the solid black lines and dashed red lines, respectively. The background symbols describe a g fib < 25.0 sample; the color-coding indicates the mean HSC/DR2 z phot measurements, and the transparency scales with the logarithm of the density. The contours and tracks are as in Figure 3.
Paper: Target Selection and Validation of DESI Emission Line Galaxies
Authors: A. Raichoor, J. Moustakas, Jeffrey A. Newman, T. Karim, S. Ahlen, Shadab Alam, S. Bailey, D. Brooks, K. Dawson, A. de la Macorra, A. de Mattia, A. Dey, Biprateep Dey, G. Dhungana, S. Eftekharzadeh, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. García-Bellido, E. Gaztañaga, S. Gontcho A Gontcho, J. Guy, K. Honscheid, M. Ishak, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, M. Manera, P. Martini, Aaron M. Meisner, Adam D. Myers, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. J. Ross, V. Ruhlmann-Kleider, C. G. Sabiu, E. F. Schlafly, D. Schlegel, Gregory Tarlé, B. A. Weaver, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Sky maps of the Galactic dust extinction (top), the imaging g-band depth (middle), and the extinction-corrected g-band depth (bottom), for the imaging data used to select the DESI ELG targets. The depths are 5σ depths for a 0.″45 radius exponential profile, typical of DESI ELG targets. The thick black line represents the 14,000 deg2 footprint covered by DESI. The Galactic plane is displayed as a solid line and the Sagittarius plane is displayed as a dashed line.
Paper: Target Selection and Validation of DESI Emission Line Galaxies
Authors: A. Raichoor, J. Moustakas, Jeffrey A. Newman, T. Karim, S. Ahlen, Shadab Alam, S. Bailey, D. Brooks, K. Dawson, A. de la Macorra, A. de Mattia, A. Dey, Biprateep Dey, G. Dhungana, S. Eftekharzadeh, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. García-Bellido, E. Gaztañaga, S. Gontcho A Gontcho, J. Guy, K. Honscheid, M. Ishak, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, M. Manera, P. Martini, Aaron M. Meisner, Adam D. Myers, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. J. Ross, V. Ruhlmann-Kleider, C. G. Sabiu, E. F. Schlafly, D. Schlegel, Gregory Tarlé, B. A. Weaver, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Cumulative distribution of the logarithm of the photometric S/N (see the text) in the selection band for the DESI Main Survey dark tracers over the nominal DESI footprints. For the ELG targets, the two Main Survey selections are shown.
Paper: Target Selection and Validation of DESI Emission Line Galaxies
Authors: A. Raichoor, J. Moustakas, Jeffrey A. Newman, T. Karim, S. Ahlen, Shadab Alam, S. Bailey, D. Brooks, K. Dawson, A. de la Macorra, A. de Mattia, A. Dey, Biprateep Dey, G. Dhungana, S. Eftekharzadeh, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. García-Bellido, E. Gaztañaga, S. Gontcho A Gontcho, J. Guy, K. Honscheid, M. Ishak, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, M. Manera, P. Martini, Aaron M. Meisner, Adam D. Myers, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. J. Ross, V. Ruhlmann-Kleider, C. G. Sabiu, E. F. Schlafly, D. Schlegel, Gregory Tarlé, B. A. Weaver, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Distribution of the fraction of reliable z spec measurements in the {FOII_SNR, Z} plane, for the 0.6 < z < 1.6 range (top), zooming in on the 1.45 < z < 1.55 range (bottom). The solid black line displays the median FOII_SNR value. The symbol transparency scales with the logarithm of the density. In both plots, the sky emission lines are displayed as black rectangles at the top of the plots, where the sky wavelength λ sky is converted to z spec = λ sky/3728 − 1 (that is, to the redshift of an [O II] doublet observed at that wavelength). The data come from about 600,000 Main ELG spectra observed in coadded reductions with 800 s < EFFTIME_SPEC < 1200 s.
Paper: Target Selection and Validation of DESI Emission Line Galaxies
Authors: A. Raichoor, J. Moustakas, Jeffrey A. Newman, T. Karim, S. Ahlen, Shadab Alam, S. Bailey, D. Brooks, K. Dawson, A. de la Macorra, A. de Mattia, A. Dey, Biprateep Dey, G. Dhungana, S. Eftekharzadeh, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. García-Bellido, E. Gaztañaga, S. Gontcho A Gontcho, J. Guy, K. Honscheid, M. Ishak, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, M. Manera, P. Martini, Aaron M. Meisner, Adam D. Myers, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. J. Ross, V. Ruhlmann-Kleider, C. G. Sabiu, E. F. Schlafly, D. Schlegel, Gregory Tarlé, B. A. Weaver, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: ELG target properties in the {FOII_SNR, DELTACHI2} plane. Top: the fraction of z spec validated by VI. Bottom: the average z spec,VI. In both plots, the slanted solid line is our criterion for selecting reliable z spec measurements, while the dashed and dotted–dashed vertical lines illustrate two threshold values for a lower cut in DELTACHI2. The symbol transparency scales with the logarithm of the density. The data come from several reductions with 200 s < EFFTIME_SPEC < 1600 s of the 3500 ELG_LOP and ELG_VLO targets with VI spectra (see the text).
Paper: Target Selection and Validation of DESI Emission Line Galaxies
Authors: A. Raichoor, J. Moustakas, Jeffrey A. Newman, T. Karim, S. Ahlen, Shadab Alam, S. Bailey, D. Brooks, K. Dawson, A. de la Macorra, A. de Mattia, A. Dey, Biprateep Dey, G. Dhungana, S. Eftekharzadeh, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. García-Bellido, E. Gaztañaga, S. Gontcho A Gontcho, J. Guy, K. Honscheid, M. Ishak, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, M. Manera, P. Martini, Aaron M. Meisner, Adam D. Myers, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. J. Ross, V. Ruhlmann-Kleider, C. G. Sabiu, E. F. Schlafly, D. Schlegel, Gregory Tarlé, B. A. Weaver, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Typical ELG spectrum, observed with eBOSS over ∼1 hr (red) and DESI over ∼15 minutes (blue). The ELG target has g fib = 23.2 mag and z spec = 0.8478. The top panel shows the full observed wavelength range, while the bottom three panels show zoom-ins on the main emission lines for the spectrum: the [O II] doublet (left), the Hβ line (middle), and the [O III] λ λ 4960, 5008 Å lines (right). The shaded regions show the estimated 1σ uncertainty on the measured flux. The spectra in the top panel are smoothed with a box of 11 pixels.
Paper: Target Selection and Validation of DESI Emission Line Galaxies
Authors: A. Raichoor, J. Moustakas, Jeffrey A. Newman, T. Karim, S. Ahlen, Shadab Alam, S. Bailey, D. Brooks, K. Dawson, A. de la Macorra, A. de Mattia, A. Dey, Biprateep Dey, G. Dhungana, S. Eftekharzadeh, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. García-Bellido, E. Gaztañaga, S. Gontcho A Gontcho, J. Guy, K. Honscheid, M. Ishak, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, M. Manera, P. Martini, Aaron M. Meisner, Adam D. Myers, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. J. Ross, V. Ruhlmann-Kleider, C. G. Sabiu, E. F. Schlafly, D. Schlegel, Gregory Tarlé, B. A. Weaver, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Sky distribution of the DESI-observed dark tiles used in this paper. They come from the following surveys: SV (black, 37 tiles), One-Percent (red, 239 tiles), and Main (2021 May–July: green, 305 tiles; 2021 September–December: orange, 973 tiles).
Paper: Target Selection and Validation of DESI Emission Line Galaxies
Authors: A. Raichoor, J. Moustakas, Jeffrey A. Newman, T. Karim, S. Ahlen, Shadab Alam, S. Bailey, D. Brooks, K. Dawson, A. de la Macorra, A. de Mattia, A. Dey, Biprateep Dey, G. Dhungana, S. Eftekharzadeh, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. García-Bellido, E. Gaztañaga, S. Gontcho A Gontcho, J. Guy, K. Honscheid, M. Ishak, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, M. Manera, P. Martini, Aaron M. Meisner, Adam D. Myers, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. J. Ross, V. Ruhlmann-Kleider, C. G. Sabiu, E. F. Schlafly, D. Schlegel, Gregory Tarlé, B. A. Weaver, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Main Survey ELG_LOP (left) and ELG_VLO (right) sample density sky maps. The density is divided by the overall average value (1940 deg−2 for the ELG_LOP sample and 460 deg−2 for the ELG_VLO sample), to display the fractional difference to the average. The thick black line represents the 14,000 deg2 footprint covered by DESI. The Galactic plane is displayed as a solid line, while the Sagittarius plane is displayed as a dashed line.