adsabs/AstroCLIMB huggingface dataset:
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Same as Figure 25, but for SN Ic-bl.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Same as Figure 18, but for SN Ib and SN Ibn subtypes.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption:                    ﹩{\mathrm{JD}}_{V\max }﹩ colors relative to V for all SESN subtypes and photometric bands for which the color at ﹩{\mathrm{JD}}_{V\max }﹩ can be measured for at least three objects. Uncertainties represent the standard deviation of the color measurements in the sample (thick lines) and magnitude uncertainties added in quadrature (thin lines). Note that the y-axis limits are restricted to (−2.1, 2.2) for readability. Errors associated with magnitude uncertainties exceed this range for SNe Ic-bl in V − r, V − R, and V − i.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Comparison of the fast-evolving SESNe from Ho23 with our GP templates of the same subtype as the spectroscopic SN classification (from top to bottom, SN IIb, SN Ib, SN Ic, SN Ic-bl).
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: GP templates for SNe Ibn in B, g, V, r, R, i, and I bands (purple curves) are plotted, along with the H17 SN Ibn r/R template. The behavior of H17's SN Ibn template is mostly consistent with our SN Ibn template within the uncertainty. A faster rise in g and r, where we have early data, is observed. However, the g data that generate this template are selected for its rapid evolution (Section 5.8), introducing a selection bias that may explain the discrepancy.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: SN Ibn GP templates in B, g, V, r, R, i, and I, along with light curves of our SN Ibn sample excluding SNe from Ho23.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Same as Figure 18, but for Ib and IIb subtypes.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Evolution of colors for each SESN subtype (Ib, IIb , Ic, Ic-bl, Ibn) between −10 and 30 days from JDmax. The most significant evolution is seen in bluer colors.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Same as Figure 18, but for IIb and Ic subtypes.
Paper: Multifilter UV to Near-infrared Data-driven Light-curve Templates for Stripped-envelope Supernovae
Authors: Somayeh Khakpash, Federica B. Bianco, Maryam Modjaz, Willow F. Fortino, Alexander Gagliano, Conor Larison, Tyler A. Pritchard
Figure caption: Same as Figure 18, but for Ib and Ic subtypes.
Paper: Exploring Unobscured Quasi-stellar Objects in the Southern Hemisphere with KS4
Authors: Yongjung Kim, Minjin Kim, Myungshin Im, Seo-Won Chang, Mankeun Jeong, Woowon Byun, Joonho Kim, Dohyeong Kim, Hyunjin Shim, Hyunmi Song
Figure caption: Color–color diagrams of the reliable sources that have SSFLAG=Null and NDITH ≥4 in the KS4 catalog. The QSO selection criteria are indicated by black lines. The blue contours map the distribution of type-1 QSOs in B. W. Lyke et al. (2020), while the red contours represent the distribution of type-2 QSOs (R. Reyes et al. 2008). The blue contour levels range from 0.5σ to 3σ at 0.5σ intervals, starting from the innermost to the outermost, whereas red contour levels range from 0.5σ to 2σ with the same increment, also moving outward from the center. The squares indicate the spectroscopically confirmed QSOs from the Milliquas v8 catalog (E. W. Flesch 2023) within our survey area. The brown circles represent the QSOs selected by our method, while the orange triangles and yellow diamonds are rejected ones due to their photometry and poor fitting results, respectively.
Paper: Exploring Unobscured Quasi-stellar Objects in the Southern Hemisphere with KS4
Authors: Yongjung Kim, Minjin Kim, Myungshin Im, Seo-Won Chang, Mankeun Jeong, Woowon Byun, Joonho Kim, Dohyeong Kim, Hyunjin Shim, Hyunmi Song
Figure caption: Histograms of the reliable sources selected by SSFLAG and NDITH_BVRI criteria across the BVRI bands. The forced photometry in the I band yields flux measurements of numerous sources beyond the 5σ imaging depths, as indicated by the vertical dotted lines in each panel. The red histograms represent the marginal reduction in source count after applying an SNR criterion in the I band. The blue histograms show the decrease in numbers when applying additional SNR criteria across the B/W1/W2/W3 bands. Note that the sudden increase in number at I ≲ 16 mag is due to the bright stars that remain after the SNR cut. The shaded regions denote the ranges of saturated magnitudes.
Paper: Exploring Unobscured Quasi-stellar Objects in the Southern Hemisphere with KS4
Authors: Yongjung Kim, Minjin Kim, Myungshin Im, Seo-Won Chang, Mankeun Jeong, Woowon Byun, Joonho Kim, Dohyeong Kim, Hyunjin Shim, Hyunmi Song
Figure caption: Sky coverage map for the KS4 data, centered on the south ecliptic pole. Areas surveyed at least four times in the BVRI bands using dithering techniques (NDITH_BVRI  ≥ 4) are marked in red. The DES survey area is shown in blue. The background represents a color composite from the Digital Sky Survey 2.
Paper: Exploring Unobscured Quasi-stellar Objects in the Southern Hemisphere with KS4
Authors: Yongjung Kim, Minjin Kim, Myungshin Im, Seo-Won Chang, Mankeun Jeong, Woowon Byun, Joonho Kim, Dohyeong Kim, Hyunjin Shim, Hyunmi Song
Figure caption: Differential number counts of KS4 QSO candidates in the ﹩i^{\prime} ﹩ band (red circles) at ∣b∣ > 10°. The gray squares represent spectroscopically identified unobscured QSOs in SDSS (B. W. Lyke et al. 2020), while the open symbols indicate incomplete bins. Similarly, the filled and open sky-blue triangles are for the DES DR2 QSO candidates (Q. Yang & Y. Shen 2023). The inset shows the number counts of KS4 QSO candidates with varying Galactic latitude limitations, compared to those of SDSS QSOs.
Paper: Exploring Unobscured Quasi-stellar Objects in the Southern Hemisphere with KS4
Authors: Yongjung Kim, Minjin Kim, Myungshin Im, Seo-Won Chang, Mankeun Jeong, Woowon Byun, Joonho Kim, Dohyeong Kim, Hyunjin Shim, Hyunmi Song
Figure caption: Example of SED-fitting results. The yellow squares are the photometric data, while the blue, red, and gray lines represent the best-fit galaxy, QSO, and star models, respectively. The χ 2 values of the models are marked in the legend.
Paper: Exploring Unobscured Quasi-stellar Objects in the Southern Hemisphere with KS4
Authors: Yongjung Kim, Minjin Kim, Myungshin Im, Seo-Won Chang, Mankeun Jeong, Woowon Byun, Joonho Kim, Dohyeong Kim, Hyunjin Shim, Hyunmi Song
Figure caption: Stacked histogram (top) and fractional distribution (bottom) of QSO candidates at ∣b∣ > 10° selected in Quaia and this work. The gray histogram represents the candidates both in Quaia and this work. The red histogram indicates the candidates only in this work. The navy, blue, and sky-blue histograms are those rejected due to NDITH, color/SNR criteria, and SED-fit results, respectively.
Paper: Exploring Unobscured Quasi-stellar Objects in the Southern Hemisphere with KS4
Authors: Yongjung Kim, Minjin Kim, Myungshin Im, Seo-Won Chang, Mankeun Jeong, Woowon Byun, Joonho Kim, Dohyeong Kim, Hyunjin Shim, Hyunmi Song
Figure caption: Changes in sky coverage depending on HEALPix levels of 11 (gray), 12 (orange), and 13 (red). Each panel presents the effective area coverage for a given HEALPix level, with areas from the n = 11 level superimposed to enable direct comparison. The unoccupied regions are attributable to the gaps between the KMTNet CCD chips, representing incomplete regions not covered by at least four dithered observations or the areas affected by bright stars.
Paper: Exploring Unobscured Quasi-stellar Objects in the Southern Hemisphere with KS4
Authors: Yongjung Kim, Minjin Kim, Myungshin Im, Seo-Won Chang, Mankeun Jeong, Woowon Byun, Joonho Kim, Dohyeong Kim, Hyunjin Shim, Hyunmi Song
Figure caption: Redshift (left) and I-band magnitude (right) distributions of Milliquas QSOs within the KS4 survey area. The top and bottom panels show the stacked histograms and the fractional distributions, respectively. The brown histograms represent the QSOs that meet our selection criteria, while the orange and yellow histograms are the rejected ones because of their photometry and poor fitting results, respectively.
Paper: Exploring Unobscured Quasi-stellar Objects in the Southern Hemisphere with KS4
Authors: Yongjung Kim, Minjin Kim, Myungshin Im, Seo-Won Chang, Mankeun Jeong, Woowon Byun, Joonho Kim, Dohyeong Kim, Hyunjin Shim, Hyunmi Song
Figure caption: Stacked histogram (top) and fractional distribution (bottom) of our QSO candidates, with classifications based on inclusion in the Gaia DR3 data set. The colors represent different classifications based on probability thresholds: red for P QSO > 0.5, orange for P Gal > 0.5, and yellow for P Star > 0.5. Dark gray indicates those within Gaia DR3 that do not meet any of the specified probability criteria, while light gray represents candidates not matched to Gaia DR3 sources.
Paper: Explicit Symplectic Integrators with Adaptive Time Steps in Curved Spacetimes
Authors: Xin Wu, Ying Wang, Wei Sun, Fuyao Liu, Dazhu Ma
Figure caption: Numerical comparisons between the methods S 2 and AS 2 integrating the chaotic photon orbit with the initial separation r = 15 of Figure 7(a). The integration step number is 105. (a) The old time steps Δτ depending on the distance r. (b) The original time τ depending on the transformation time w or s. (c) Accuracy of Hamiltonian K.
Paper: The MOST Hosts Survey: Spectroscopic Observation of the Host Galaxies of ∼40,000 Transients Using DESI
Authors: Maayane T. Soumagnac, Peter Nugent, Robert A. Knop, Anna Y. Q. Ho, William Hohensee, Autumn Awbrey, Alexis Andersen, Greg Aldering, Matan Ventura, Jessica N. Aguilar, Steven Ahlen, Segev Y. Benzvi, David Brooks, Dillon Brout, Todd Claybaugh, Tamara M. Davis, Kyle Dawson, Axel de la Macorra, Arjun Dey, Biprateep Dey, Peter Doel, Kelly A. Douglass, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Or Graur, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Cullan Howlett, Alex G. Kim, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Dustin Lang, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jundan Nie, Antonella Palmese, David Parkinson, Claire Poppett, Francisco Prada, Fei Qin, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, David J. Schlegel, Michael Schubnell, Joseph H. Silber, Gregory Tarlé, Benjamin A. Weaver, Zhimin Zhou
Figure caption: Left panel: a histogram of the difference in inferred distance modulus between those obtained by the DESI MOST Hosts project and those obtained from ZTF, either from preexisting galaxy catalogs (blue, totaling 1064 SNe Ia) or from those obtained by the lower-resolution SEDm (red, totaling 593 SNe Ia). The increase in the scatter is ∼0.08 mag for those obtained by SEDm. Right panel: a histogram of the difference in velocities obtained with the DESI MOST Hosts project and with ZTF using the SEDm, including 1548 with an SNID (S. Blondin & J. L. Tonry 2007) measurement from M. Rigault et al. (2024). The Gaussian that best fits this histogram corresponds to 1σ = 986 km s−1.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The MOST Hosts Survey: Spectroscopic Observation of the Host Galaxies of ∼40,000 Transients Using DESI
Authors: Maayane T. Soumagnac, Peter Nugent, Robert A. Knop, Anna Y. Q. Ho, William Hohensee, Autumn Awbrey, Alexis Andersen, Greg Aldering, Matan Ventura, Jessica N. Aguilar, Steven Ahlen, Segev Y. Benzvi, David Brooks, Dillon Brout, Todd Claybaugh, Tamara M. Davis, Kyle Dawson, Axel de la Macorra, Arjun Dey, Biprateep Dey, Peter Doel, Kelly A. Douglass, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Or Graur, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Cullan Howlett, Alex G. Kim, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Dustin Lang, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jundan Nie, Antonella Palmese, David Parkinson, Claire Poppett, Francisco Prada, Fei Qin, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, David J. Schlegel, Michael Schubnell, Joseph H. Silber, Gregory Tarlé, Benjamin A. Weaver, Zhimin Zhou
Figure caption: Example of multiple potential host identifications. The left panel shows the Legacy survey image, with the location of the transient (yellow) at α = 67.°217 and δ = −9.°379. The middle panel shows the hosts proposed by our algorithm as likely potential hosts, before filtering out Tractor shreds. The hosts annotated as “E” and “B” are Tractor shreds: Tractor modeled the arm of the galaxy annotated as “C” with multiple smaller galaxies, a well-known and documented behavior that is visible in the right panel, where we show the Tractor model for this image. “E” and “B” were filtered out by the procedure described in Section 2.4, leaving us with the hosts “A,” “C,” and “D” as the potential hosts. The host annotated “A” is probably not the correct host, but the algorithm was tweaked conservatively, resulting in a higher likelihood of proposing wrong hosts rather than missing correct ones. Although “C” seems like the most plausible host, without additional information, such as the redshift, it is hard to exclude “D” as the correct host.
Paper: The MOST Hosts Survey: Spectroscopic Observation of the Host Galaxies of ∼40,000 Transients Using DESI
Authors: Maayane T. Soumagnac, Peter Nugent, Robert A. Knop, Anna Y. Q. Ho, William Hohensee, Autumn Awbrey, Alexis Andersen, Greg Aldering, Matan Ventura, Jessica N. Aguilar, Steven Ahlen, Segev Y. Benzvi, David Brooks, Dillon Brout, Todd Claybaugh, Tamara M. Davis, Kyle Dawson, Axel de la Macorra, Arjun Dey, Biprateep Dey, Peter Doel, Kelly A. Douglass, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Or Graur, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Cullan Howlett, Alex G. Kim, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Dustin Lang, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jundan Nie, Antonella Palmese, David Parkinson, Claire Poppett, Francisco Prada, Fei Qin, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, David J. Schlegel, Michael Schubnell, Joseph H. Silber, Gregory Tarlé, Benjamin A. Weaver, Zhimin Zhou
Figure caption: Preliminary Hubble diagram of a subset of the SN Ia hosts observed so far with the MOST Hosts project. The plot shows SNe from the MOST Hosts sample that have hosts observed by DESI and that are part of the ZTF BTS (D. A. Perley et al. 2020). The redshifts are the DESI redshifts of the host galaxy of the SN. Red points are ones that do not pass the cuts ∣c∣ < 0.3, ∣x 1∣ < 3, σ  c  < 0.2, ﹩{\sigma }_{{x}_{1}}\lt 1﹩ (B. Popovic et al. 2021); these objects were not included in the fit to Equation (1). Error bars on m bcor include a 0.15 mag intrinsic dispersion. Inset: histogram of residuals of the data points that passed the cuts relative to the fit Hubble law.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The MOST Hosts Survey: Spectroscopic Observation of the Host Galaxies of ∼40,000 Transients Using DESI
Authors: Maayane T. Soumagnac, Peter Nugent, Robert A. Knop, Anna Y. Q. Ho, William Hohensee, Autumn Awbrey, Alexis Andersen, Greg Aldering, Matan Ventura, Jessica N. Aguilar, Steven Ahlen, Segev Y. Benzvi, David Brooks, Dillon Brout, Todd Claybaugh, Tamara M. Davis, Kyle Dawson, Axel de la Macorra, Arjun Dey, Biprateep Dey, Peter Doel, Kelly A. Douglass, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Or Graur, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Cullan Howlett, Alex G. Kim, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Dustin Lang, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jundan Nie, Antonella Palmese, David Parkinson, Claire Poppett, Francisco Prada, Fei Qin, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, David J. Schlegel, Michael Schubnell, Joseph H. Silber, Gregory Tarlé, Benjamin A. Weaver, Zhimin Zhou
Figure caption: Description of the list of transients. The left panel shows the fraction of transients originating from each of the surveys used. The right panel shows the types of the transients for which a classification is available (26.7% of all transients in our list).
Paper: The MOST Hosts Survey: Spectroscopic Observation of the Host Galaxies of ∼40,000 Transients Using DESI
Authors: Maayane T. Soumagnac, Peter Nugent, Robert A. Knop, Anna Y. Q. Ho, William Hohensee, Autumn Awbrey, Alexis Andersen, Greg Aldering, Matan Ventura, Jessica N. Aguilar, Steven Ahlen, Segev Y. Benzvi, David Brooks, Dillon Brout, Todd Claybaugh, Tamara M. Davis, Kyle Dawson, Axel de la Macorra, Arjun Dey, Biprateep Dey, Peter Doel, Kelly A. Douglass, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Or Graur, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Cullan Howlett, Alex G. Kim, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Dustin Lang, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jundan Nie, Antonella Palmese, David Parkinson, Claire Poppett, Francisco Prada, Fei Qin, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, David J. Schlegel, Michael Schubnell, Joseph H. Silber, Gregory Tarlé, Benjamin A. Weaver, Zhimin Zhou
Figure caption: Histogram of host redshifts observed by DESI that will be included in DR1. Each transient is included once in the histogram; in cases where more than one potential host for a transient has been observed by DESI, one of the observations is chosen randomly for the histogram. We show in red the distribution for hosts of transients for which a classification exists and in blue the distribution for hosts for which no classification is known.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The MOST Hosts Survey: Spectroscopic Observation of the Host Galaxies of ∼40,000 Transients Using DESI
Authors: Maayane T. Soumagnac, Peter Nugent, Robert A. Knop, Anna Y. Q. Ho, William Hohensee, Autumn Awbrey, Alexis Andersen, Greg Aldering, Matan Ventura, Jessica N. Aguilar, Steven Ahlen, Segev Y. Benzvi, David Brooks, Dillon Brout, Todd Claybaugh, Tamara M. Davis, Kyle Dawson, Axel de la Macorra, Arjun Dey, Biprateep Dey, Peter Doel, Kelly A. Douglass, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Or Graur, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Cullan Howlett, Alex G. Kim, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Dustin Lang, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jundan Nie, Antonella Palmese, David Parkinson, Claire Poppett, Francisco Prada, Fei Qin, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, David J. Schlegel, Michael Schubnell, Joseph H. Silber, Gregory Tarlé, Benjamin A. Weaver, Zhimin Zhou
Figure caption: Peak absolute magnitude of classified and unclassified ZTF objects, calculated from DESI redshift measurements, plotted against duration.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The MOST Hosts Survey: Spectroscopic Observation of the Host Galaxies of ∼40,000 Transients Using DESI
Authors: Maayane T. Soumagnac, Peter Nugent, Robert A. Knop, Anna Y. Q. Ho, William Hohensee, Autumn Awbrey, Alexis Andersen, Greg Aldering, Matan Ventura, Jessica N. Aguilar, Steven Ahlen, Segev Y. Benzvi, David Brooks, Dillon Brout, Todd Claybaugh, Tamara M. Davis, Kyle Dawson, Axel de la Macorra, Arjun Dey, Biprateep Dey, Peter Doel, Kelly A. Douglass, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Or Graur, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Cullan Howlett, Alex G. Kim, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Dustin Lang, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jundan Nie, Antonella Palmese, David Parkinson, Claire Poppett, Francisco Prada, Fei Qin, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, David J. Schlegel, Michael Schubnell, Joseph H. Silber, Gregory Tarlé, Benjamin A. Weaver, Zhimin Zhou
Figure caption: Description of the algorithm used to select one or several potential hosts.
Paper: The MOST Hosts Survey: Spectroscopic Observation of the Host Galaxies of ∼40,000 Transients Using DESI
Authors: Maayane T. Soumagnac, Peter Nugent, Robert A. Knop, Anna Y. Q. Ho, William Hohensee, Autumn Awbrey, Alexis Andersen, Greg Aldering, Matan Ventura, Jessica N. Aguilar, Steven Ahlen, Segev Y. Benzvi, David Brooks, Dillon Brout, Todd Claybaugh, Tamara M. Davis, Kyle Dawson, Axel de la Macorra, Arjun Dey, Biprateep Dey, Peter Doel, Kelly A. Douglass, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Or Graur, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Cullan Howlett, Alex G. Kim, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Dustin Lang, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jundan Nie, Antonella Palmese, David Parkinson, Claire Poppett, Francisco Prada, Fei Qin, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, David J. Schlegel, Michael Schubnell, Joseph H. Silber, Gregory Tarlé, Benjamin A. Weaver, Zhimin Zhou
Figure caption: Distribution of MOST Hosts candidates on the sky. Gray dots represent everything in the MOST Hosts target list. Blue dots represent candidates for which at least one host has been observed as of MOST Hosts DR1. (At this scale, it is impossible to separate multiple hosts for the same candidate.)