Candidate Periodically Variable Quasars from the Dark Energy Survey and the Sloan Digital Sky Survey. (arXiv:2008.12329v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Yu-Ching Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_X/0/1/0/all/0/1">Xin Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liao_W/0/1/0/all/0/1">Wei-Ting Liao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holgado_A/0/1/0/all/0/1">A. Miguel Holgado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guo_H/0/1/0/all/0/1">Hengxiao Guo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruendl_R/0/1/0/all/0/1">Robert A. Gruendl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morganson_E/0/1/0/all/0/1">Eric Morganson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shen_Y/0/1/0/all/0/1">Yue Shen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_K/0/1/0/all/0/1">Kaiwen Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">Tim M. C. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguena_M/0/1/0/all/0/1">Michel Aguena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allam_S/0/1/0/all/0/1">Sahar Allam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_S/0/1/0/all/0/1">Santiago Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_E/0/1/0/all/0/1">Emmanuel Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhargava_S/0/1/0/all/0/1">Sunayana Bhargava</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_D/0/1/0/all/0/1">David Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_D/0/1/0/all/0/1">David L. Burke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosell_A/0/1/0/all/0/1">Aurelio Carnero Rosell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carollo_D/0/1/0/all/0/1">Daniela Carollo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kind_M/0/1/0/all/0/1">Matias Carrasco Kind</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_J/0/1/0/all/0/1">Jorge Carretero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costanzi_M/0/1/0/all/0/1">Matteo Costanzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_L/0/1/0/all/0/1">Luiz N. da Costa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_T/0/1/0/all/0/1">Tamara M. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vicente_J/0/1/0/all/0/1">Juan De Vicente</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desai_S/0/1/0/all/0/1">Shantanu Desai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diehl_H/0/1/0/all/0/1">H. Thomas Diehl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doel_P/0/1/0/all/0/1">Peter Doel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Everett_S/0/1/0/all/0/1">Spencer Everett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flaugher_B/0/1/0/all/0/1">Brenna Flaugher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Friedel_D/0/1/0/all/0/1">Douglas Friedel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frieman_J/0/1/0/all/0/1">Joshua Frieman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Bellido_J/0/1/0/all/0/1">Juan García-Bellido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaztanaga_E/0/1/0/all/0/1">Enrique Gaztanaga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glazebrook_K/0/1/0/all/0/1">Karl Glazebrook</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruen_D/0/1/0/all/0/1">Daniel Gruen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gutierrez_G/0/1/0/all/0/1">Gaston Gutierrez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hinton_S/0/1/0/all/0/1">Samuel R. Hinton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hollowood_D/0/1/0/all/0/1">Devon L. Hollowood</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+James_D/0/1/0/all/0/1">David J. James</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_A/0/1/0/all/0/1">Alex G. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuehn_K/0/1/0/all/0/1">Kyler Kuehn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuropatkin_N/0/1/0/all/0/1">Nikolay Kuropatkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lewis_G/0/1/0/all/0/1">Geraint F. Lewis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lidman_C/0/1/0/all/0/1">Christopher Lidman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lima_M/0/1/0/all/0/1">Marcos Lima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maia_M/0/1/0/all/0/1">Marcio A. G. Maia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+March_M/0/1/0/all/0/1">Marisa March</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshall_J/0/1/0/all/0/1">Jennifer L. Marshall</a>, et al. (16 additional authors not shown)
Periodically variable quasars have been suggested as close binary
supermassive black holes. We present a systematic search for periodic light
curves in 625 spectroscopically confirmed quasars with a median redshift of 1.8
in a 4.6 deg$^2$ overlapping region of the Dark Energy Survey Supernova
(DES-SN) fields and the Sloan Digital Sky Survey Stripe 82 (SDSS-S82). Our
sample has a unique 20-year long multi-color ($griz$) light curve enabled by
combining new DES-SN Y6 observations with archival SDSS-S82 data. The deep
imaging allows us to search for periodic light curves in less luminous quasars
(down to $r{sim}$23.5 mag) powered by less massive black holes (with masses
$gtrsim10^{8.5}M_{odot}$) at high redshift for the first time. We find five
candidates with significant (at $>$99.74% level in at least two bands)
periodicity with observed periods of $sim$3–5 years (i.e., 1–2 years in rest
frame) having $sim$4–6 cycles spanned by the observations. If all five
candidates are periodically variable quasars, this translates into a detection
rate of ${sim}0.8^{+0.5}_{-0.3}$% (assuming 1$sigma$ Poisson error) or
${sim}1.1^{+0.7}_{-0.5}$ quasar per deg$^2$. Our detection rate is 4–80 times
larger than those found by previous searches using shallower surveys over
larger areas. This apparent discrepancy is likely caused by differences in the
quasar populations being probed and the survey data qualities. We discuss
implications of our results on the future direct detection of low-frequency
gravitational waves. Continued photometric monitoring will further assess the
robustness and characteristics of these candidate periodic quasars to determine
their physical origins.
Periodically variable quasars have been suggested as close binary
supermassive black holes. We present a systematic search for periodic light
curves in 625 spectroscopically confirmed quasars with a median redshift of 1.8
in a 4.6 deg$^2$ overlapping region of the Dark Energy Survey Supernova
(DES-SN) fields and the Sloan Digital Sky Survey Stripe 82 (SDSS-S82). Our
sample has a unique 20-year long multi-color ($griz$) light curve enabled by
combining new DES-SN Y6 observations with archival SDSS-S82 data. The deep
imaging allows us to search for periodic light curves in less luminous quasars
(down to $r{sim}$23.5 mag) powered by less massive black holes (with masses
$gtrsim10^{8.5}M_{odot}$) at high redshift for the first time. We find five
candidates with significant (at $>$99.74% level in at least two bands)
periodicity with observed periods of $sim$3–5 years (i.e., 1–2 years in rest
frame) having $sim$4–6 cycles spanned by the observations. If all five
candidates are periodically variable quasars, this translates into a detection
rate of ${sim}0.8^{+0.5}_{-0.3}$% (assuming 1$sigma$ Poisson error) or
${sim}1.1^{+0.7}_{-0.5}$ quasar per deg$^2$. Our detection rate is 4–80 times
larger than those found by previous searches using shallower surveys over
larger areas. This apparent discrepancy is likely caused by differences in the
quasar populations being probed and the survey data qualities. We discuss
implications of our results on the future direct detection of low-frequency
gravitational waves. Continued photometric monitoring will further assess the
robustness and characteristics of these candidate periodic quasars to determine
their physical origins.
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