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1. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author

Adhikari, Susmita, Shin, Tae-hyeon, Jain, Bhuvnesh, Hilton, Matt, Baxter, Eric, Chang, Chihway, Wechsler, Risa H, Battaglia, Nick, Bond, J Richard, Bocquet, Sebastian, DeRose, Joseph, Choi, Steve K, Devlin, Mark, Dunkley, Jo, Evrard, August E, Ferraro, Simone, Hill, J Colin, Hughes, John P, Gallardo, Patricio A, Lokken, Martine, MacInnis, Amanda, McMahon, Jeffrey, Madhavacheril, Mathew S, Nati, Frederico, Newburgh, Laura B, Niemack, Michael D, Page, Lyman A, Palmese, Antonella, Partridge, Bruce, Rozo, Eduardo, Rykoff, Eli, Salatino, Maria, Schillaci, Alessandro, Sehgal, Neelima, Sifón, Cristóbal, To, Chun-Hao, Wollack, Ed, Wu, Hao-Yi, Xu, Zhilei, Aguena, Michel, Allam, Sahar, Amon, Alexandra, Annis, James, Avila, Santiago, Bacon, David, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L, Rosell, Aurelio C, Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Choi, Ami, Costanzi, Matteo, Costa, Luiz N da, Vicente, Juan De, Desai, Shantanu, Diehl, Thomas H, Doel, Peter, Everett, Spencer, Ferrero, Ismael, Ferté, Agnès, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, García-Bellido, Juan, Gaztanaga, Enrique, Gruen, Daniel, Gruendl, Robert A, Gschwend, Julia, Gutierrez, Gaston, Hartley, Will G, Hinton, Samuel R, Hollowood, Devon L, Honscheid, Klaus, James, David J, Jeltema, Tesla, Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, Ofer, Lima, Marcos, Maia, Marcio AG, Marshall, Jennifer L, Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Ogando, Ricardo LC, Paz-Chinchón, Francisco, Malagón, Andrés Plazas, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, and Suchyta, Eric

Subjects
Particle and Plasma Physics, astro-ph.GA, Molecular, Nuclear, Astronomy & Astrophysics, Atomic, Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev--Zeldovich (SZ) effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius for the complete galaxy sample is consistent with theoretical measurements from CDM-only simulations, and is located at $2.4^{+0.3}_{-0.4}$ Mpc $h^{-1}$. We split the sample based on galaxy color and find significant differences in the profile shapes. Red galaxies and those in the green valley show a splashback-like minimum in their slope profile consistent with theoretical predictions, while the bluest galaxies show a weak feature that appears at a smaller radius. We develop a mapping of galaxies to subhalos in $N$-body simulations by splitting subhalos based on infall time onto the cluster halos. We find that the location of the steepest slope and differences in the shapes of the profiles can be mapped to differences in the average time of infall of galaxies of different colors. The minima of the slope in the galaxy profiles trace a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time for galaxies of different colours, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in their clusters for over $3.2 ~\rm Gyrs$, green galaxies about $2.2 ~\rm Gyrs$, while blue galaxies have been accreted most recently and have not reached apocenter. Using the information from the complete radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching in clusters occurs after a delay of about a gigayear, and that galaxies quench rapidly thereafter with an exponential timescale of $0.6$ Gyr.

Published
2021

2. Dwarf AGNs from Optical Variability for the Origins of Seeds (DAVOS): Insights from the Dark Energy Survey Deep Fields

Author

Burke, Colin J., Liu, Xin, Shen, Yue, Phadke, Kedar A., Yang, Qian, Hartley, Will G., Harrison, Ian, Palmese, Antonella, Guo, Hengxiao, Zhang, Kaiwen, Kron, Richard, Turner, David J., Giles, Paul A., Lidman, Christopher, Chen, Yu-Ching, Gruendl, Robert A., Choi, Ami, Amon, Alexandra, Sheldon, Erin, Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bertin, E., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., García-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Reil, K., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wilkinson, R. D., Collaboration, DES, Burke, Colin J., Liu, Xin, Shen, Yue, Phadke, Kedar A., Yang, Qian, Hartley, Will G., Harrison, Ian, Palmese, Antonella, Guo, Hengxiao, Zhang, Kaiwen, Kron, Richard, Turner, David J., Giles, Paul A., Lidman, Christopher, Chen, Yu-Ching, Gruendl, Robert A., Choi, Ami, Amon, Alexandra, Sheldon, Erin, Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bertin, E., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., García-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wilkinson, R. D., and Des, Collaboration

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, black hole physics, galaxies active, galaxies dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, black hole physic, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

We present a sample of 706, $z < 1.5$ active galactic nuclei (AGNs) selected from optical photometric variability in three of the Dark Energy Survey (DES) deep fields (E2, C3, and X3) over an area of 4.64 deg$^2$. We construct light curves using difference imaging aperture photometry for resolved sources and non-difference imaging PSF photometry for unresolved sources, respectively, and characterize the variability significance. Our DES light curves have a mean cadence of 7 days, a 6 year baseline, and a single-epoch imaging depth of up to $g \sim 24.5$. Using spectral energy distribution (SED) fitting, we find 26 out of total 706 variable galaxies are consistent with dwarf galaxies with a reliable stellar mass estimate ($M_{\ast}, 21 pages, 22 figures incl. 3 appendices; accepted for publication in MNRAS

Published
2021
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3. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author

Adhikari, Susmita, Shin, Tae-hyeon, Jain, Bhuvnesh, Hilton, Matt, Baxter, Eric, Chang, Chihway, Wechsler, Risa H., Battaglia, Nick, Bond, J. Richard, Bocquet, Sebastian, DeRose, Joseph, Choi, Steve K., Devlin, Mark, Dunkley, Jo, Evrard, August E., Ferraro, Simone, Hill, J. Colin, Hughes, John P., Gallardo, Patricio A., Lokken, Martine, MacInnis, Amanda, McMahon, Jeffrey, Madhavacheril, Mathew S., Nati, Frederico, Newburgh, Laura B., Niemack, Michael D., Page, Lyman A., Palmese, Antonella, Partridge, Bruce, Rozo, Eduardo, Rykoff, Eli, Salatino, Maria, Schillaci, Alessandro, Sehgal, Neelima, Sif��n, Crist��bal, To, Chun-Hao, Wollack, Ed, Wu, Hao-Yi, Xu, Zhilei, Aguena, Michel, Allam, Sahar, Amon, Alexandra, Annis, James, Avila, Santiago, Bacon, David, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L., Rosell, Aurelio C., Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Choi, Ami, Costanzi, Matteo, da Costa, Luiz N., De Vicente, Juan, Desai, Shantanu, Diehl, Thomas H., Doel, Peter, Everett, Spencer, Ferrero, Ismael, Fert��, Agn��s, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Garc��a-Bellido, Juan, Gaztanaga, Enrique, Gruen, Daniel, Gruendl, Robert A., Gschwend, Julia, Gutierrez, Gaston, Hartley, Will G., Hinton, Samuel R., Hollowood, Devon L., Honscheid, Klaus, James, David J., Jeltema, Tesla, Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, Ofer, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Ogando, Ricardo L. C., Paz-Chinch��n, Francisco, Malag��n, Andr��s Plazas, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Suchyta, Eric, Swanson, Molly E. C., Varga, Tamas N., Wilkinson, Reese D., Zhang, Yuanyuan, Austermann, Jason E., Beall, James A., Becker, Daniel T., Denison, Edward V., Duff, Shannon M., Hilton, Gene C., Hubmayr, Johannes, Ullom, Joel N., Van Lanen, Jeff, Vale, Leila R., Collaboration, DES, Collaboration, ACT, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), Adhikari, S, Shin, T, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, R, Battaglia, N, Bond, J, Bocquet, S, Choi, S, Derose, J, Devlin, M, Dunkley, J, Evrard, A, Ferraro, S, Hill, J, Hughes, J, Gallardo, P, Lokken, M, Macinnis, A, Madhavacheril, M, Mcmahon, J, Nati, F, Newburgh, L, Niemack, M, Page, L, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, To, C, Wollack, E, Wu, H, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, D, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, A, Costanzi, M, Da Costa, L, Vicente, J, Desai, S, Diehl, T, Doel, P, Everett, S, Ferrero, I, Ferte, A, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R, Gschwend, J, Gutierrez, G, Hartley, W, Hinton, S, Hollowood, D, Honscheid, K, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M, Marshall, J, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchon, F, Malagon, A, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, E. C. Swanson, M, Varga, T, Wilkinson, R, Zhang, Y, Austermann, J, Beall, J, Becker, D, Denison, E, Duff, S, Hilton, G, Hubmayr, J, Ullom, J, Lanen, J, Vale, L, Adhikari, S., Shin, T. -H., Jain, B., Hilton, M., Baxter, E., Chang, C., Wechsler, R. H., Battaglia, N., Bond, J. R., Bocquet, S., Choi, S. K., Derose, J., Devlin, M., Dunkley, J., Evrard, A. E., Ferraro, S., Hill, J. C., Hughes, J. P., Gallardo, P. A., Lokken, M., Macinnis, A., Madhavacheril, M. S., Mcmahon, J., Nati, F., Newburgh, L. B., Niemack, M. D., Page, L. A., Palmese, A., Partridge, B., Rozo, E., Rykoff, E., Salatino, M., Schillaci, A., Sehgal, N., Sifon, C., C. -H., To, Wollack, E., H. -Y., Wu, Xu, Z., Aguena, M., Allam, S., Amon, A., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. C., Kind, M. C., Carretero, J., Castander, F. J., Choi, A., Costanzi, M., Da Costa, L. N., Vicente, J. D., Desai, S., Diehl, T. H., Doel, P., Everett, S., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., L. C. Ogando R., Paz-Chinchon, F., Malagon, A. P., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., E. C. Swanson M., Varga, T. N., Wilkinson, R. D., Zhang, Y., Austermann, J. E., Beall, J. A., Becker, D. T., Denison, E. V., Duff, S. M., Hilton, G. C., Hubmayr, J., Ullom, J. N., Lanen, J. V., and Vale, L. R.

Subjects
Galaxy dark matter halos, 010308 nuclear & particles physics, FOS: Physical sciences, Cold dark matter, Astronomy and Astrophysics, Galaxy clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology, SZ effect, Galaxy cluster, Surveys, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxy evolution, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy kinematics
Abstract

Adhikari, S., et al. (DES and ACT Collaboration), We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev-Zel'dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at 2.4-0.4+0.3 Mpc h-1. We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr., The DES Data Management System is supported by the NSF under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Unionʼs Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2)

Published
2021

4. Faint submillimeter galaxies identified through their optical/near-infrared colors: 1. Spatial clustering and halo masses

Author

Chen (陳建州), Chian-Chou, Smail, Ian, Swinbank, A.M., Simpson, James M., Almaini, Omar, Conselice, Christopher J., Hartley, Will G., Mortlock, Alice, Simpson, Chris, and Wilkinson, Aaron

Subjects
submillimeter: galaxies, galaxies: high-redshift, cosmology: observations, largescalestructure of universe, galaxies: formation, galaxies: evolution
Abstract

The properties of submillimeter galaxies (SMGs) that are fainter than the confusion limit of blank-field single-dish surveys (S850  2 mJy) are poorly constrained. Using a newly developed color selection technique, Optical-Infrared Triple Color (OIRTC), that has been shown to successfully select such faint SMGs, we identify a sample of 2938 OIRTC-selected galaxies, dubbed Triple Color Galaxies (TCGs), in the UKIDSS-UDS field. We show that these galaxies have a median 850 μm flux of S850 = 0.96 +/- 0.04 mJy (equivalent to a star formation rate SFR ~60–100 M yr−1 based on spectral energy distribution fitting), representing the first large sample of faint SMGs that bridges the gap between bright SMGs and normal star-forming galaxies in S850 and LIR. We assess the basic properties of TCGs and their relationship with other galaxy populations at z ~ 2. We measure the two-point autocorrelation function for this population and derive a typical halo mass of log10(Mhalo) = -12.9+0.2-0.3, 12.7+0.1,-0.2, and 12.9+0.2,-0,3 h-1 M at z = 1–2, 2–3, and 3–5, respectively. Together with the bright SMGs (S850 >/~ 2 mJy) and a comparison sample of less far-infrared luminous star-forming galaxies, we find a lack of dependence between spatial clustering and S850 (or SFR), suggesting that the difference between these populations may lie in their local galactic environment. Lastly, on the scale of ~8–17 kpc at 1 < z < 5 we find a tentative enhancement of the clustering of TCGs over the comparison star-forming galaxies, suggesting that some faint SMGs are physically associated pairs, perhaps reflecting a merging origin in their triggering.

Published
2016

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