adsabs/AstroCLIMB huggingface dataset:
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: Example of a region with Galactic dust clouds causing extreme extinction variations at small scales, which are imprinted in the ELG_LOP target sample (yellow circles). The cutout is centered at (R.A., decl.) = (31.°40, 20.°66) and it is 0.°4 wide.
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_LOP (solid lines) and ELG_VLO (dashed lines) total target magnitude normalized cumulative distributions in the g band (left), r band (middle), and z band (right). For the g band, we also display the fiber magnitude distributions (red lines).
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 target density variations, with foreground (top) and imaging seeing (middle), as well as depth (bottom). The South-DES decl. < −30° region has been excluded. We consider bins with at least 100 HEALPix 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: Main Survey ELG_VLO target density variations, with foreground (top) and imaging seeing (middle), as well as depth (bottom). The South-DES decl. < −30° region has been excluded. We consider bins with at least 100 HEALPix pixels.
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: Number densities of massive QGs as a function of redshift at 2 < z < 5. We report the number densities calculated for our sample (dark red stars) in redshifts bins of 2 < z < 3 (log(M */M ⊙) > 10), 3 < z < 4 (log(M */M ⊙) > 10.6), and 4 < z < 5 (log(M */M ⊙) > 10.6). The errors on the number densities include both Poisson noise and cosmic variance added in quadrature. We plot number densities from Straatman et al. (2014), Schreiber et al. (2018), Merlin et al. (2019), Carnall et al. (2020), Shahidi et al. (2020), Weaver et al. (2022), the extended sample from Girelli et al. (2019), and Carnall et al. (2022). Also shown are number densities for the FLARES and EAGLE simulations for massive galaxies (log(M */M ⊙) > 10.6) at two quiescent selection thresholds (log10(sSFR/Gyr−1) < [–1, –2]) (Lovell et al. 2022), as well as QGs from the SHARK simulation at two mass (log(M */M ⊙) > [10, 10.6]) and sSFR selection thresholds (log10(sSFR/Gyr−1) < [–1, –2])
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 column: SHARK-simulated galaxies in different color planes. GMM/NUV − VJ (this work, top) and UVJ (middle) color diagrams for massive (log(M */M ⊙ > 10)) galaxies in the SHARK simulation (gray), with QGs found by each selection method as red (blue) hexagons and galaxies missed by both selection methods as red (blue) crosses. The bottom panel shows the receiver operator characteristic (ROC) curve for the trained GMM as a function of quiescent probability (p(q)) threshold. The area under the curve (AUC), which represents the percentage probability of correctly classifying QGs, is reported, as well as the p(q) threshold, which is calculated as the geometric mean (shown on the figure as the colored red circle on the red curve). The false-positive rate (FPR) and true-positive rate (FPR) are also presented for the Whitaker et al. (2012) UVJ selection (blue star). Middle column: same as left column but at z = 3. Right column: same as left column but at z = 4.
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: Top row: NUV − VJ-selected QGs at 2 < z < 3 (dark red, left figure) shown in NUV − VJ space, UVJ space, and NUVrJ space. Middle row: NUVrJ-selected QGs (middle figure, light blue) shown in NUV − VJ and UVJ color diagrams. Bottom row: UVJ-selected QGs (right figure, dark blue) shown in NUV − VJ and NUVrJ color diagrams. For each panel the overlap is given, defined as the number of galaxies selected by that selection method divided by the number of galaxies selected by the main selection method for that row. In the first row, we show the GMM-selected sample (dark red) at 2 < z < 3 in the NUV − VJ diagram, NUVrJ diagram, and UVJ diagram. The second row shows the NUVrJ-selected sample in NUVrJ (light blue) as well as the other two color–color diagrams, and the third row shows the UVJ-selected sample in UVJ as well as in the other two color–color diagrams (dark blue).
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 − VJ diagram with the 2 < z < 3 fitting sample colored by p(q)50%, which is the median of the bootstrapped quiescent probability distribution based on the GMM. Right: same but for the 3 < z < 5 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: 10″ × 10″ postage-stamp cutouts from selected bands in the optical to NIR scaled by ±3 rms (left) and corresponding best-fit SEDs (right) for three QG candidates selected using the NUV − VJ method, taken from the main sample. The observed photometric points are shown as black circles (any with S/N <2 in gray), and the best-fit model is shown in blue. The rest-frame NUV, U, V, J photometry is shown by the orange circles. The p(z) is shown to the right of each SED in yellow, along with its best-fit photometric redshift, stellar mass, and quiescent probability median value (P(q)50).
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: Top: median smoothed rest-frame SED for the GMM/NUV − VJ-selected quiescent sample at 3 < z < 5. Rest-frame photometry for all galaxies is shown in gray, while the median per band and the associated 16th and 84th percentiles (error bars) are shown in dark gray. The median best-fit (smoothed) model is shown in red. The median model photometry per band is shown by the open face circles. At the top left the sample median properties (number, median K  s -band magnitude, median log(stellar mass), median log(SFR), median log(sSSFR)) are shown, as well as the standard deviation.
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: Signal-to-noise ratio (S/N) as a function of redshift at 3.0 < z < 5.0 for IRAC Channel 3 (top) and IRAC Channel 4 (bottom) for the whole massive sample (gray). The average S/N for each channel is shown binned in redshift for the entire massive sample (blue dots) and the extended quiescent sample (red stars). The worst performance is at 4.5 < z < 5.0 for both channels.
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:  gzK diagram for all galaxies in the combined UVISTA and HSC area with g, z and K S/N > 3. Stars (black dots) occupy a locus across the lower part of the diagram, whereas galaxies (shown in green and purple dots) tend to occupy a wider spread of colors.
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: Same as Figure 6 but for 3 < z < 5.
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: Comparison of the HSC/DR2 z phot to the DESI Main Survey ELG z spec measurements, using ∼175,000 matched targets with a z spec passing our reliability criterion of Equation (1). Left: scatter plots color-coded according to the average HSC risk parameter (see the text); the solid lines in the bottom panel are the median values of Δz  =  (z phot − z spec)/(1 + z spec) for three subsamples—all the matches (black), the 50% lower risk parameter values (cyan), and the 25% lower risk parameter values (red), with the shaded regions showing the 1.48 × MAD(Δz) values. Right: redshift distributions for these three subsamples; in each panel, the filled (empty) histogram is for the DESI z spec (HSC z phot). The DESI z spec distribution with no cut on risk is displayed via the black hatched histogram.
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: Illustration of the [O II] doublet in the ELG_LOP spectra. The left (middle) panel displays four spectra at z = 1.3 (z = 1.55) for EFFTIME_SPEC = 1.0 ks, with typical FOII_SNR values for the considered redshift. The right panel displays the same four z = 1.55 targets, but as observed with EFFTIME_SPEC = 6.6 ks. The thick red line shows the observed flux, the blue-filled region shows the flux uncertainty, and the black line is the best-fit model. The [O II] doublet wavelengths are displayed as vertical dashed black lines. The sky emission line wavelengths are indicated with the vertical blue dotted lines.
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: Redshift distributions for the Main ELG_LOP (top) and ELG_VLO (bottom) samples, split by footprint. The reported densities are the expected densities of the observed ELG targets providing a reliable z spec (see the text for more details). The vertical dashed lines emphasize the relevant redshift ranges for the ELGs: z = 0.6, z = 1.1, and z = 1.6.
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: Redshift difference dv for 19,000 pairs of independent repeat observations of Main ELG_LOP targets with 0.6 < z < 1.6. Top: dv as a function of FOII_SNR; the black dashed line (dv = 1000 km s−1) illustrates the threshold used to identify the pairs with catastrophic measurements (red dots). Bottom: normalized distribution of the dv values; the red curve illustrates a reasonable representation of the distribution, from the weighted sum of two Gaussian distributions, with widths of 5 and 20 km s−1. The data come from independent repeat observations from the SV, One-Percent, and Main Surveys (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: Efficiency as a function of color and magnitude, in the 0.6 < z < 1.6 (top) and 1.1 < z < 1.6 (bottom) range. The left column shows the g − r vs. r − z diagram, the middle column shows the (g − r) + 1.2 × (r − z) vs. g fib diagram, and the right column shows the g tot vs. g fib plane. The Main ELG_LOP and ELG_VLO selections are displayed as the solid dark lines and the dashed red lines, respectively; the SV ELG selection is displayed as a thick solid gray line. The data come from different reductions of SV ELG-only tiles, with 800 s < EFFTIME_SPEC < 1200 s, representative of the Main Survey EFFTIME_SPEC values.
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: [O II] flux limit as a function of z spec for FOII_SNR = 7 ELG spectra. Each point marks an ELG spectrum, with the solid black line displaying the median values. The horizontal dashed blue lines are the median values for the dz = 0.2 bins, while the horizontal dashed red lines are the DESI requirements. The sky emission lines are displayed as the black rectangles at the tops of the plots, as in Figure 13. The data come from 15,400 Main ELG spectra, observed in coadded reductions with 800 s < EFFTIME_SPEC < 1200 s and 6.8 < FOII_SNR < 7.2.
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: Fraction of catastrophic z spec measurements for the Main ELG_LOP targets with 0.6 < z < 1.6 and a reliable z spec (Equation (1)), as a function of EFFTIME_SPEC (top) and z spec (bottom). The gray histograms show the distributions of the probed values, and the dashed lines highlight a catastrophic z spec fraction of 1%. The data come from different reductions of the 2900 ELG_LOP targets with VI.
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 Main selection efficiency in the 0.6 < z < 1.6 and 1.1 < z < 1.6 ranges, as a function of EFFTIME_SPEC, for the three surveys (the SV, One-Percent, and Main Surveys). Top: split per survey. Bottom: all surveys together. The histograms show the EFFTIME_SPEC normalized distributions.