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1. An Extended Catalogue of galaxy morphology using Deep Learning in Southern Photometric Local Universe Survey Data Release 3

Author

Bom, C. R., Cortesi, A., Ribeiro, U., Dias, L. O., Kelkar, K., Castelli, A. V. Smith, Santana-Silva, L., Silva, V., Gonçalves, T. S., Abramo, L. R., Lima, E. V. R., Almeida-Fernandes, F., Espinosa, L., Li, L., Buzzo, M. L., de Oliveira, C. Mendes, Sodré Jr., L., Alvarez-Candal, A., Grossi, M., Telles, E., Torres-Flores, S., Werner, S. V., Kanaan, A., Ribeiro, T., and Schoenell, W.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The morphological diversity of galaxies is a relevant probe of galaxy evolution and cosmological structure formation. However, in large sky surveys, even the morphological classification of galaxies into two classes, like late-type (LT) and early-type (ET), still represents a significant challenge. In this work we present a Deep Learning (DL) based morphological catalog built from images obtained by the Southern Photometric Local Universe Survey (S-PLUS) Data Release 3 (DR3). Our DL method achieves an precision rate of 98.5$\%$ in accurately distinguishing between spiral, as part of the larger category of late type (LT) galaxies, and elliptical, belonging to early type (ET) galaxies. Additionally, we have implemented a secondary classifier that evaluates the quality of each galaxy stamp, which allows to select only high-quality images when studying properties of galaxies on the basis of their DL morphology. From our LT/ET catalog of galaxies, we recover the expected color--magnitude diagram in which LT galaxies display bluer colors than ET ones. Furthermore, we also investigate the clustering of galaxies based on their morphology, along with their relationship to the surrounding environment. As a result, we deliver a full morphological catalog with $164314$ objects complete up to $r_{petro}<18$, covering $\sim 1800$ deg$^2$, including a significant area of the Southern hemisphere that was not covered by previous morphology catalogues., Comment: 22 pages, 24 figures

Published
2023

2. Intracluster light in the core of z~2 galaxy proto-clusters

Author

Werner, S. V., Hatch, N. A., Matharu, J., Gonzalez, A. H., Bahé, Y. M., Mei, S., Noirot, G., and Wylezalek, D.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Intracluster light is thought to originate from stars that were ripped away from their parent galaxies by gravitational tides and galaxy interactions during the build up of the cluster. The stars from such interactions will accumulate over time, so semi-analytic models suggest that the abundance of intracluster stars is negligible in young proto-clusters at z~2 and grows to around a quarter of the stellar mass in the oldest, most mature clusters. In contrast to these theoretical expectations, we report on the detection of intracluster light within two proto-clusters at z=2 using deep HST images. We use the colour of the intracluster light to estimate its mass-to-light ratio in annuli around the brightest cluster galaxies (BCG), up to a radius of 100 kpc. We find that $54\pm5$% and $71\pm3$% of the stellar mass in these regions is located more than 10 kpc away from the BCGs in the two proto-clusters. This low concentration is similar to BCGs in lower redshift clusters, and distinct from other massive proto-cluster galaxies. This suggests that intracluster stars are already present within the core 100 kpc of proto-clusters. We compare these observations to the Hydrangea hydrodynamical galaxy cluster simulations and find that intracluster stars are predicted to be a generic feature of group-sized halos at z=2. These intracluster stars will gradually move further away from the BCG as the proto-cluster assembles into a cluster., Comment: 14 pages, 9 figures, accepted for publication in MNRAS

Published
2023
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3. S-PLUS DR1 galaxy clusters and groups catalogue using PzWav

Author

Werner, S. V., Cypriano, E. S., Gonzalez, A. H., de Oliveira, C. Mendes, Araya-Araya, P., Doubrawa, L., de Oliveira, R. Lopes, Lopes, P. A. A., Vitorelli, A. Z., Brambila, D., Costa-Duarte, M., Telles, E., Kanaan, A., Ribeiro, T., Schoenell, W., Gonçalves, T. S., Menéndez-Delmestre, K., Bom, C. R., and Nakazono, L.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a catalogue of 4499 groups and clusters of galaxies from the first data release of the multi-filter (5 broad, 7 narrow) Southern Photometric Local Universe Survey (S-PLUS). These groups and clusters are distributed over 273 deg$^2$ in the Stripe 82 region. They are found using the PzWav algorithm, which identifies peaks in galaxy density maps that have been smoothed by a cluster scale difference-of-Gaussians kernel to isolate clusters and groups. Using a simulation-based mock catalogue, we estimate the purity and completeness of cluster detections: at S/N>3.3 we define a catalogue that is 80% pure and complete in the redshift range 0.1 10^{14}$ M$_\odot$. We also assessed the accuracy of the catalogue in terms of central positions and redshifts, finding scatter of $\sigma_R=12$ kpc and $\sigma_z=8.8 \times 10^{-3}$, respectively. Moreover, less than 1% of the sample suffers from fragmentation or overmerging. The S-PLUS cluster catalogue recovers ~80% of all known X-ray and Sunyaev-Zel'dovich selected clusters in this field. This fraction is very close to the estimated completeness, thus validating the mock data analysis and paving an efficient way to find new groups and clusters of galaxies using data from the ongoing S-PLUS project. When complete, S-PLUS will have surveyed 9300 deg$^{2}$ of the sky, representing the widest uninterrupted areas with narrow-through-broad multi-band photometry for cluster follow-up studies., Comment: 17 pages, 15 figures, paper accepted for publication by MNRAS

Published
2022
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4. Satellite quenching was not important for z$\sim$1 clusters: most quenching occurred during infall

Author

Werner, S. V., Hatch, N. A., Muzzin, A., van der Burg, R. F. J., Balogh, M. L., Rudnick, G., and Wilson, G.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We quantify the relative importance of environmental quenching versus pre-processing in $z\sim1$ clusters by analysing the infalling galaxy population in the outskirts of 15 galaxy clusters at $0.810^{11}M_{\odot}$ were quenched prior to infall, whilst up to half of lower mass galaxies were environmentally quenched after passing the virial radius. This means most of the massive quiescent galaxies in $z\sim1$ clusters were self-quenched or pre-processed prior to infall., Comment: 13 pages, 11 figures, paper accepted for publication by MNRAS

Published
2021
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5. Assessing the photometric redshift precision of the S-PLUS survey: the Stripe-82 as a test-case

Author

Molino, A., Costa-Duarte, M. V., Sampedro, L., Herpich, F. R., Sodré Jr., L., de Oliveira, C. Mendes, Schoenell, W., Barbosa, C. E., Queiroz, C., Lima, E. V. R., Azanha, L., Muñoz-Elgueta, N., Ribeiro, T., Kanaan, A., Hernandez-Jimenez, J. A., Cortesi, A., Akras, S., de Oliveira, R. Lopes, Torres-Flores, S., Lima-Dias, C., Castellon, J. L. Nilo, Damke, G., Alvarez-Candal, A., Jiménez-Teja, Y., Coelho, P., Pereira, E., Montero-Dorta, A. D., Benítez, N., Gonçalves, T. S., Santana-Silva, L., Werner, S. V., Almeida, L. A., Lopes, P. A. A., Chies-Santos, A. L., Telles, E., de Souza, Thom, C., R., Gonçalves, D. R., de Souza, R. S., Makler, M., Placco, V. M., Nakazono, L. M. I., Saito, R. K., Overzier, R. A., and Abramo, L. R.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

In this paper we present a thorough discussion about the photometric redshift (photo-z) performance of the Southern Photometric Local Universe Survey (S-PLUS). This survey combines a 7 narrow + 5 broad passband filter system, with a typical photometric-depth of r$\sim$21 AB. For this exercise, we utilize the Data Release 1 (DR1), corresponding to 336 deg$^{2}$ from the Stripe-82 region. We rely on the \texttt{BPZ2} code to compute our estimates, using a new library of SED models, which includes additional templates for quiescent galaxies. When compared to a spectroscopic redshift control sample of $\sim$100k galaxies, we find a precision of $\sigma_{z}<$0.8\%, $<$2.0\% or $<$3.0\% for galaxies with magnitudes r$<$17, $<$19 and $<$21, respectively. A precision of 0.6\% is attained for galaxies with the highest \texttt{Odds} values. These estimates have a negligible bias and a fraction of catastrophic outliers inferior to 1\%. We identify a redshift window (i.e., 0.26$

Published
2019
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6. The Southern Photometric Local Universe Survey (S-PLUS): improved SEDs, morphologies and redshifts with 12 optical filters

Author

de Oliveira, C. Mendes, Ribeiro, T., Schoenell, W., Kanaan, A., Overzier, R. A., Molino, A., Sampedro, L., Coelho, P., Barbosa, C. E., Cortesi, A., Costa-Duarte, M. V., Herpich, F. R., Hernandez-Jimenez, J. A., Placco, V. M., Xavier, H. S., Abramo, L. R., Saito, R. K., Chies-Santos, A. L., Ederoclite, A., de Oliveira, R. Lopes, Gonçalves, D. R., Akras, S., Almeida, L. A., Almeida-Fernandes, F., Beers, T. C., Bonatto, C., Bonoli, S., Cypriano, E. S., de Lima, Erik V. R., de Souza, R. S., de Souza, G. Fabiano, Ferrari, F., Gonçalves, T. S., Gonzalez, A. H., Gutiérrez-Soto, L. A., Hartmann, E. A., Jaffe, Y., Kerber, L. O., Lima-Dias, C., Lopes, P. A. A., Menendez-Delmestre, K., Nakazono, L. M. I., Novais, P. M., Ortega-Minakata, R. A., Pereira, E. S., Perottoni, H. D., Queiroz, C., Reis, R. R. R., Santos, W. A., Santos-Silva, T., Santucci, R. M., Barbosa, C. L., Siffert, B. B., Sodré Jr., L., Torres-Flores, S., Westera, P., Whitten, D. D., Alcaniz, J. S., Alonso-García, Javier, Alencar, S., Alvarez-Candal, A., Amram, P., Azanha, L., Barbá, R. H., Bernardinelli, P. H., Fernandes, M. Borges, Branco, V., Brito-Silva, D., Buzzo, M. L., Caffer, J., Campillay, A., Cano, Z., Carvano, J. M., Castejon, M., Fernandes, R. Cid, Dantas, M. L. L., Daflon, S., Damke, G., de la Reza, R., de Azevedo, L. J. de Melo, De Paula, D. F., Diem, K. G., Donnerstein, R., Dors, O. L., Dupke, R., Eikenberry, S., Escudero, Carlos G., Faifer, Favio R., Farías, H., Fernandes, B., Fernandes, C., Fontes, S., Galarza, A., Hirata, N. S. T., Katena, L., Gregorio-Hetem, J., Hernández-Fernández, J. D., Izzo, L., Arancibia, M. Jaque, Jatenco-Pereira, V., Jiménez-Teja, Y., Kann, D. A., Krabbe, A. C., Labayru, C., Lazzaro, D., Neto, G. B. Lima, Lopes, Amanda R., Magalhães, R., Makler, M., de Menezes, R., Miralda-Escudé, J., Monteiro-Oliveira, R., Montero-Dorta, A. D., Muñoz-Elgueta, N., Nemmen, R. S., Castellón, J. L. Nilo, Oliveira, A. S., Ortíz, D., Pattaro, E., Pereira, C. B., Quint, B., Riguccini, L., Pinto, H. J. Rocha, Rodrigues, I., Roig, F., Rossi, S., Saha, Kanak, Santos, R., Müller, A. Schnorr, Sesto, Leandro A., Silva, R., Castelli, Analía V. Smith, Teixeira, Ramachrisna, Telles, E., de Souza, R. C. Thom, Thöne, C., Trevisan, M., Postigo, A. de Ugarte, Urrutia-Viscarra, F., Veiga, C. H., Vika, M., Vitorelli, A. Z., Werle, A., Werner, S. V., and Zaritsky, D.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

The Southern Photometric Local Universe Survey (S-PLUS) is imaging ~9300 deg^2 of the celestial sphere in twelve optical bands using a dedicated 0.8 m robotic telescope, the T80-South, at the Cerro Tololo Inter-American Observatory, Chile. The telescope is equipped with a 9.2k by 9.2k e2v detector with 10 um pixels, resulting in a field-of-view of 2 deg^2 with a plate scale of 0.55"/pixel. The survey consists of four main subfields, which include two non-contiguous fields at high Galactic latitudes (8000 deg^2 at |b| > 30 deg) and two areas of the Galactic plane and bulge (for an additional 1300 deg^2). S-PLUS uses the Javalambre 12-band magnitude system, which includes the 5 u, g, r, i, z broad-band filters and 7 narrow-band filters centered on prominent stellar spectral features: the Balmer jump/[OII], Ca H+K, H-delta, G-band, Mg b triplet, H-alpha, and the Ca triplet. S-PLUS delivers accurate photometric redshifts (delta_z/(1+z) = 0.02 or better) for galaxies with r < 20 AB mag and redshift < 0.5, thus producing a 3D map of the local Universe over a volume of more than 1 (Gpc/h)^3. The final S-PLUS catalogue will also enable the study of star formation and stellar populations in and around the Milky Way and nearby galaxies, as well as searches for quasars, variable sources, and low-metallicity stars. In this paper we introduce the main characteristics of the survey, illustrated with science verification data highlighting the unique capabilities of S-PLUS. We also present the first public data release of ~336 deg^2 of the Stripe-82 area, which is available at http://datalab.noao.edu/splus., Comment: Updated to reflect the published version (MNRAS, 489, 241). For a short introductory video of the S-PLUS project, see https://youtu.be/yc5kHrHU9Jk - The S-PLUS Data Release 1 is available at http://datalab.noao.edu/splus

Published
2019
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7. An extended catalogue of galaxy morphology using deep learning in southern photometric local universe survey data release 3

Author

Bom, C R, primary, Cortesi, A, additional, Ribeiro, U, additional, Dias, L O, additional, Kelkar, K, additional, Smith Castelli, A V, additional, Santana-Silva, L, additional, Lopes-Silva, V, additional, Gonçalves, T S, additional, Abramo, L R, additional, Lima, E V R, additional, Almeida-Fernandes, F, additional, Espinosa, L, additional, Li, L, additional, Buzzo, M L, additional, Mendes de Oliveira, C, additional, Sodré, L, additional, Ferrari, F, additional, Alvarez-Candal, A, additional, Grossi, M, additional, Telles, E, additional, Torres-Flores, S, additional, Werner, S V, additional, Kanaan, A, additional, Ribeiro, T, additional, and Schoenell, W, additional

Published
2023
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10. S-PLUS DR1 galaxy clusters and groups catalogue using PzWav

Author

Werner, S V, primary, Cypriano, E S, additional, Gonzalez, A H, additional, Mendes de Oliveira, C, additional, Araya-Araya, P, additional, Doubrawa, L, additional, Lopes de Oliveira, R, additional, Lopes, P A A, additional, Vitorelli, A Z, additional, Brambila, D, additional, Costa-Duarte, M, additional, Telles, E, additional, Kanaan, A, additional, Ribeiro, T, additional, Schoenell, W, additional, Gonçalves, T S, additional, Menéndez-Delmestre, K, additional, Bom, C R, additional, and Nakazono, L, additional

Published
2022
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11. Satellite quenching was not important for z ?1 clusters: Most quenching occurred during infall

Author

Werner, S. V., Hatch, N. A., Muzzin, A., Balogh, M. L., Rudnick, G., and Wilson, G.

Subjects
Space and Planetary Science, Astronomy and Astrophysics
Abstract

We quantify the relative importance of environmental quenching versus pre-processing in z ?1 clusters by analysing the infalling galaxy population in the outskirts of 15 galaxy clusters at 0.8 < z < 1.4 drawn from the GOGREEN and GCLASS surveys. We find significant differences between the infalling galaxies and a control sample; in particular, an excess of massive quiescent galaxies in the infalling region. These massive infalling galaxies likely reside in larger dark matter haloes than similar-mass control galaxies because they have twice as many satellite galaxies. Furthermore, these satellite galaxies are distributed in an NFW profile with a larger scale radius compared to the satellites of the control galaxies. Based on these findings, we conclude that it may not be appropriate to use 'field' galaxies as a substitute for infalling pre-cluster galaxies when calculating the efficiency and mass dependence of environmental quenching in high-redshift clusters. By comparing the quiescent fraction of infalling galaxies at 1 < R/R2001011 Mpdbl were quenched prior to infall, while up to half of lower mass galaxies were environmentally quenched after passing the virial radius. This means most of the massive quiescent galaxies in z ?1 clusters were self-quenched or pre-processed prior to infall.

Published
2022

12. S-PLUS DR1 galaxy clusters and groups catalogue using PzWav.

Author

Werner, S V, Cypriano, E S, Gonzalez, A H, Mendes de Oliveira, C, Araya-Araya, P, Doubrawa, L, Lopes de Oliveira, R, Lopes, P A A, Vitorelli, A Z, Brambila, D, Costa-Duarte, M, Telles, E, Kanaan, A, Ribeiro, T, Schoenell, W, Gonçalves, T S, Menéndez-Delmestre, K, Bom, C R, and Nakazono, L

Subjects
*GALAXY clusters, *CATALOGS, *CATALOGING, *LARGE scale structure (Astronomy), *DATA release
Abstract

We present a catalogue of 4499 groups and clusters of galaxies from the first data release of the multi-filter (5 broad, 7 narrow) Southern Photometric Local Universe Survey (S-PLUS). These groups and clusters are distributed over 273 deg2 in the Stripe 82 region. They are found using the PzWav algorithm, which identifies peaks in galaxy density maps that have been smoothed by a cluster scale difference-of-Gaussians kernel to isolate clusters and groups. Using a simulation-based mock catalogue, we estimate the purity and completeness of cluster detections: at S/N > 3.3, we define a catalogue that is 80 per cent pure and complete in the redshift range 0.1 < z < 0.4, for clusters with M200 > 1014 M⊙. We also assessed the accuracy of the catalogue in terms of central positions and redshifts, finding scatter of σR = 12 kpc and σz = 8.8 × 10−3, respectively. Moreover, less than 1 per cent of the sample suffers from fragmentation or overmerging. The S-PLUS cluster catalogue recovers ∼80 per cent of all known X-ray and Sunyaev-Zel'dovich selected clusters in this field. This fraction is very close to the estimated completeness, thus validating the mock data analysis and paving an efficient way to find new groups and clusters of galaxies using data from the ongoing S-PLUS project. When complete, S-PLUS will have surveyed 9300 deg2 of the sky, representing the widest uninterrupted areas with narrow-through-broad multi-band photometry for cluster follow-up studies. [ABSTRACT FROM AUTHOR]

Published
2023
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14. Assessing the photometric redshift precision of the S-PLUS survey: the Stripe-82 as a test-case

Author

Molino, A, primary, Costa-Duarte, M V, additional, Sampedro, L, additional, Herpich, F R, additional, Sodré, L, additional, Mendes de Oliveira, C, additional, Schoenell, W, additional, Barbosa, C E, additional, Queiroz, C, additional, Lima, E V R, additional, Azanha, L, additional, Muñoz-Elgueta, N, additional, Ribeiro, T, additional, Kanaan, A, additional, Hernandez-Jimenez, J A, additional, Cortesi, A, additional, Akras, S, additional, Lopes de Oliveira, R, additional, Torres-Flores, S, additional, Lima-Dias, C, additional, Castellon, J L Nilo, additional, Damke, G, additional, Alvarez-Candal, A, additional, Jiménez-Teja, Y, additional, Coelho, P, additional, Pereira, E, additional, Montero-Dorta, A D, additional, Benítez, N, additional, Gonçalves, T S, additional, Santana-Silva, L, additional, Werner, S V, additional, Almeida, L A, additional, Lopes, P A A, additional, Chies-Santos, A L, additional, Telles, E, additional, de Souza, Thom, additional, C, R, additional, Gonçalves, D R, additional, de Souza, R S, additional, Makler, M, additional, Buzzo, M L, additional, Placco, V M, additional, Nakazono, L M I, additional, Saito, R K, additional, Overzier, R A, additional, and Abramo, L R, additional

Published
2020
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15. Satellite quenching was not important for z ∼ 1 clusters: most quenching occurred during infall.

Author

Werner, S V, Hatch, N A, Muzzin, A, van der Burg, R F J, Balogh, M L, Rudnick, G, and Wilson, G

Subjects
*GALAXY clusters, *DARK matter, *GALACTIC evolution, *CLUSTER sampling, *GALAXIES
Abstract

We quantify the relative importance of environmental quenching versus pre-processing in z ∼ 1 clusters by analysing the infalling galaxy population in the outskirts of 15 galaxy clusters at 0.8 < z < 1.4 drawn from the GOGREEN and GCLASS surveys. We find significant differences between the infalling galaxies and a control sample; in particular, an excess of massive quiescent galaxies in the infalling region. These massive infalling galaxies likely reside in larger dark matter haloes than similar-mass control galaxies because they have twice as many satellite galaxies. Furthermore, these satellite galaxies are distributed in an NFW profile with a larger scale radius compared to the satellites of the control galaxies. Based on these findings, we conclude that it may not be appropriate to use 'field' galaxies as a substitute for infalling pre-cluster galaxies when calculating the efficiency and mass dependence of environmental quenching in high-redshift clusters. By comparing the quiescent fraction of infalling galaxies at 1 < R /R200<3 to the cluster sample (R /R200<1) we find that almost all quiescent galaxies with masses >1011 M⊙ were quenched prior to infall, while up to half of lower mass galaxies were environmentally quenched after passing the virial radius. This means most of the massive quiescent galaxies in z ∼ 1 clusters were self-quenched or pre-processed prior to infall. [ABSTRACT FROM AUTHOR]

Published
2022
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16. The Southern Photometric Local Universe Survey (S-PLUS): improved SEDs, morphologies, and redshifts with 12 optical filters

Author

Mendes de Oliveira, C, primary, Ribeiro, T, additional, Schoenell, W, additional, Kanaan, A, additional, Overzier, R A, additional, Molino, A, additional, Sampedro, L, additional, Coelho, P, additional, Barbosa, C E, additional, Cortesi, A, additional, Costa-Duarte, M V, additional, Herpich, F R, additional, Hernandez-Jimenez, J A, additional, Placco, V M, additional, Xavier, H S, additional, Abramo, L R, additional, Saito, R K, additional, Chies-Santos, A L, additional, Ederoclite, A, additional, Lopes de Oliveira, R, additional, Gonçalves, D R, additional, Akras, S, additional, Almeida, L A, additional, Almeida-Fernandes, F, additional, Beers, T C, additional, Bonatto, C, additional, Bonoli, S, additional, Cypriano, E S, additional, Vinicius-Lima, E, additional, de Souza, R S, additional, Fabiano de Souza, G, additional, Ferrari, F, additional, Gonçalves, T S, additional, Gonzalez, A H, additional, Gutiérrez-Soto, L A, additional, Hartmann, E A, additional, Jaffe, Y, additional, Kerber, L O, additional, Lima-Dias, C, additional, Lopes, P A A, additional, Menendez-Delmestre, K, additional, Nakazono, L M I, additional, Novais, P M, additional, Ortega-Minakata, R A, additional, Pereira, E S, additional, Perottoni, H D, additional, Queiroz, C, additional, Reis, R R R, additional, Santos, W A, additional, Santos-Silva, T, additional, Santucci, R M, additional, Barbosa, C L, additional, Siffert, Beatriz B, additional, Sodré, L, additional, Torres-Flores, S, additional, Westera, P, additional, Whitten, D D, additional, Alcaniz, J S, additional, Alonso-García, Javier, additional, Alencar, S, additional, Alvarez-Candal, A, additional, Amram, P, additional, Azanha, L, additional, Barbá, R H, additional, Bernardinelli, P H, additional, Borges Fernandes, M, additional, Branco, V, additional, Brito-Silva, D, additional, Buzzo, M L, additional, Caffer, J, additional, Campillay, A, additional, Cano, Z, additional, Carvano, J M, additional, Castejon, M, additional, Cid Fernandes, R, additional, Dantas, M L L, additional, Daflon, S, additional, Damke, G, additional, de la Reza, R, additional, de Melo de Azevedo, L J, additional, De Paula, D F, additional, Diem, K G, additional, Donnerstein, R, additional, Dors, O L, additional, Dupke, R, additional, Eikenberry, S, additional, Escudero, Carlos G, additional, Faifer, Favio R, additional, Farías, H, additional, Fernandes, B, additional, Fernandes, C, additional, Fontes, S, additional, Galarza, A, additional, Hirata, N S T, additional, Katena, L, additional, Gregorio-Hetem, J, additional, Hernández-Fernández, J D, additional, Izzo, L, additional, Jaque Arancibia, M, additional, Jatenco-Pereira, V, additional, Jiménez-Teja, Y, additional, Kann, D A, additional, Krabbe, A C, additional, Labayru, C, additional, Lazzaro, D, additional, Lima Neto, G B, additional, Lopes, Amanda R, additional, Magalhães, R, additional, Makler, M, additional, de Menezes, R, additional, Miralda-Escudé, J, additional, Monteiro-Oliveira, R, additional, Montero-Dorta, A D, additional, Muñoz-Elgueta, N, additional, Nemmen, R S, additional, Nilo Castellón, J L, additional, Oliveira, A S, additional, Ortíz, D, additional, Pattaro, E, additional, Pereira, C B, additional, Quint, B, additional, Riguccini, L, additional, Rocha Pinto, H J, additional, Rodrigues, I, additional, Roig, F, additional, Rossi, S, additional, Saha, Kanak, additional, Santos, R, additional, Schnorr Müller, A, additional, Sesto, Leandro A, additional, Silva, R, additional, Smith Castelli, Analia V, additional, Teixeira, R, additional, Telles, E, additional, Thom de Souza, R C, additional, Thöne, C, additional, Trevisan, M, additional, de Ugarte Postigo, A, additional, Urrutia-Viscarra, F, additional, Veiga, C H, additional, Vika, M, additional, Vitorelli, A Z, additional, Werle, A, additional, Werner, S V, additional, and Zaritsky, D, additional

Published
2019
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17. The Southern Photometric Local Universe Survey (S-PLUS): improved SEDs, morphologies, and redshifts with 12 optical filters

Author

Universidad de La Serena (Chile), Centro de Estudios de Física del Cosmos de Aragón, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Financiadora de Estudos e Projetos (Brasil), National Science Foundation (US), Southern Office of Aerospace Research and Development (US), Consejo Superior de Investigaciones Científicas (España), Ministerio de Economía y Competitividad (España), European Commission, Universidad Nacional Autónoma de México, Alfred P. Sloan Foundation, National Aeronautics and Space Administration (US), Ministry of Education, Culture, Sports, Science and Technology (Japan), Max Planck Society, Higher Education Funding Council for England, American Museum of Natural History, Leibniz Institute for Astrophysics Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University (US), Joint Institute for Nuclear Astrophysics - Center for the Evolution of the Elements (US), Kavli Institute for Particle Astrophysics and Cosmology, Chinese Academy of Sciences, Los Alamos National Laboratory, Max Planck Institute for Astronomy, Max Planck Institute for Astrophysics, New Mexico State University, The Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, U.S. Naval Observatory, University of Washington, Fermilab, Institute for Advanced Study (Germany), Johns Hopkins University, de Oliveira, C. M., Ribeiro, T., Schoenell, W., Kanaan, A., Overzier, R. A., Molino, A., Sampedro, L., Coelho, P., Barbosa, Carlos Eduardo, Cortesi, A., Costa-Duarte, M. V., Brito-Silva, D., Daflon, S., Buzzo, M. L., Farias, H., Hernandez-Fernandez, J. D., Kann, D.A., Damke, G., De Paula, D. F., Dors, O. L., Escudero, C. G., Montero-Dorta, A. D., Fernandes, C., Nemmen, R. S., Katena, L., Oliveira, A. S., Arancibia, M. J., Pattaro, E., Labayru, C., Quint, B., Jatenco-Pereira, V., Rodrigues, I., Riguccini, L., Lazzaro, D., Saha, K., Roig-Roig, Ferran, Neto, G. B. L., Sesto, L. A., Santos, R., Lopes, A. R., Teixeira, R., Silva, R., Magalhães, Regina, Munoz-Elgueta, N., Trevisan, M., de Souza, R. C. T., Makler, M., Castellon, J. L. Nilo, Vika, M., Urrutia-Viscarra, F., de Menezes, R., Ortiz, D., Herpich, F.R., Werle, A., Telles, E., Miralda-Escudé, Jordi, Pereira, C. B., Monteiro-Oliveira, R., Placco, V. M., Ugarte Postigo, Antonio de, Vitorelli, A. Z., Hernández-Jiménez, J.A., Pinto, H. J. R., Rossi, S., Muller, A. S., Castelli, A. V. S., Beers, T. C., Thöne, Cristina Carina, Bonoli, Silvia, Veiga, C. H., Vinicius-Lima, E., Werner, S. V., de Souza, G. F., Xavier, H. S., Gonzalez, A. H., Zaritsky, D., Jaffe, Y., Gutiérrez-Soto, L. A., Abramo, L. R., Lopes, PAA, Kerber, L. O., Saito, R. K., Novais, P. M., Menéndez-Delmestre, Karín, Chies-Santos, A.L., Queiroz, C., Pereira, E. S., Ederoclite, Alessandro, Bonatto, C., Santucci, R. M., Santos, W. A., de Oliveira, R. L., Cypriano, E. S., Westera, P., Siffert, B. B., Gonçalves, D. R., de Souza, RS, Akras, S., Alcaniz, Jailson S., Reis, R. R. R., Almeida, L. A., Ferrari, F., Almeida-Fernandes, F., Ortega-Minakata, R. A., Barbosa, C. L., Whitten, DD, Gonçalves, T. S., Hartmann, EA, Lima-Dias, C., Nakazono, L. M. I., Perottoni, H. D., Caffer, J., Santos-Silva, T., Cano, Z., Sodre, L., Castejon, M., Alonso-Garcia, J., Dantas, M. L. L., Torres-Flores, S., de la Reza, R., Alencar, S., Diem, K. G., de Azevedo, L. J. D., Alvarez-Candal, A., Dupke, Renato A., Donnerstein, R., Amram, P., Faifer, F. R., Eikenberry, S., Azanha, L., Fontes, S., Fernandes, B., Barbá, R. H., Campillay, A., Gregorio-Hetem, J., Hirata, N. S. T., Bernardinelli, P. H., Carvano, J.M., Jiménez-Teja, Y., Izzo, L., Fernandes, M. B., Fernandes, R. C., Branco, V., Krabbe, A. C., Galarza, A., Universidad de La Serena (Chile), Centro de Estudios de Física del Cosmos de Aragón, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Financiadora de Estudos e Projetos (Brasil), National Science Foundation (US), Southern Office of Aerospace Research and Development (US), Consejo Superior de Investigaciones Científicas (España), Ministerio de Economía y Competitividad (España), European Commission, Universidad Nacional Autónoma de México, Alfred P. Sloan Foundation, National Aeronautics and Space Administration (US), Ministry of Education, Culture, Sports, Science and Technology (Japan), Max Planck Society, Higher Education Funding Council for England, American Museum of Natural History, Leibniz Institute for Astrophysics Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University (US), Joint Institute for Nuclear Astrophysics - Center for the Evolution of the Elements (US), Kavli Institute for Particle Astrophysics and Cosmology, Chinese Academy of Sciences, Los Alamos National Laboratory, Max Planck Institute for Astronomy, Max Planck Institute for Astrophysics, New Mexico State University, The Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, U.S. Naval Observatory, University of Washington, Fermilab, Institute for Advanced Study (Germany), Johns Hopkins University, de Oliveira, C. M., Ribeiro, T., Schoenell, W., Kanaan, A., Overzier, R. A., Molino, A., Sampedro, L., Coelho, P., Barbosa, Carlos Eduardo, Cortesi, A., Costa-Duarte, M. V., Brito-Silva, D., Daflon, S., Buzzo, M. L., Farias, H., Hernandez-Fernandez, J. D., Kann, D.A., Damke, G., De Paula, D. F., Dors, O. L., Escudero, C. G., Montero-Dorta, A. D., Fernandes, C., Nemmen, R. S., Katena, L., Oliveira, A. S., Arancibia, M. J., Pattaro, E., Labayru, C., Quint, B., Jatenco-Pereira, V., Rodrigues, I., Riguccini, L., Lazzaro, D., Saha, K., Roig-Roig, Ferran, Neto, G. B. L., Sesto, L. A., Santos, R., Lopes, A. R., Teixeira, R., Silva, R., Magalhães, Regina, Munoz-Elgueta, N., Trevisan, M., de Souza, R. C. T., Makler, M., Castellon, J. L. Nilo, Vika, M., Urrutia-Viscarra, F., de Menezes, R., Ortiz, D., Herpich, F.R., Werle, A., Telles, E., Miralda-Escudé, Jordi, Pereira, C. B., Monteiro-Oliveira, R., Placco, V. M., Ugarte Postigo, Antonio de, Vitorelli, A. Z., Hernández-Jiménez, J.A., Pinto, H. J. R., Rossi, S., Muller, A. S., Castelli, A. V. S., Beers, T. C., Thöne, Cristina Carina, Bonoli, Silvia, Veiga, C. H., Vinicius-Lima, E., Werner, S. V., de Souza, G. F., Xavier, H. S., Gonzalez, A. H., Zaritsky, D., Jaffe, Y., Gutiérrez-Soto, L. A., Abramo, L. R., Lopes, PAA, Kerber, L. O., Saito, R. K., Novais, P. M., Menéndez-Delmestre, Karín, Chies-Santos, A.L., Queiroz, C., Pereira, E. S., Ederoclite, Alessandro, Bonatto, C., Santucci, R. M., Santos, W. A., de Oliveira, R. L., Cypriano, E. S., Westera, P., Siffert, B. B., Gonçalves, D. R., de Souza, RS, Akras, S., Alcaniz, Jailson S., Reis, R. R. R., Almeida, L. A., Ferrari, F., Almeida-Fernandes, F., Ortega-Minakata, R. A., Barbosa, C. L., Whitten, DD, Gonçalves, T. S., Hartmann, EA, Lima-Dias, C., Nakazono, L. M. I., Perottoni, H. D., Caffer, J., Santos-Silva, T., Cano, Z., Sodre, L., Castejon, M., Alonso-Garcia, J., Dantas, M. L. L., Torres-Flores, S., de la Reza, R., Alencar, S., Diem, K. G., de Azevedo, L. J. D., Alvarez-Candal, A., Dupke, Renato A., Donnerstein, R., Amram, P., Faifer, F. R., Eikenberry, S., Azanha, L., Fontes, S., Fernandes, B., Barbá, R. H., Campillay, A., Gregorio-Hetem, J., Hirata, N. S. T., Bernardinelli, P. H., Carvano, J.M., Jiménez-Teja, Y., Izzo, L., Fernandes, M. B., Fernandes, R. C., Branco, V., Krabbe, A. C., and Galarza, A.

Abstract

The Southern Photometric Local Universe Survey (S-PLUS) is imaging similar to 9300 deg(2) of the celestial sphere in 12 optical bands using a dedicated 0.8mrobotic telescope, the T80-South, at the Cerro Tololo Inter-american Observatory, Chile. The telescope is equipped with a 9.2k x 9.2k e2v detector with 10 mu m pixels, resulting in a field of view of 2 deg(2) with a plate scale of 0.55 arcsec pixel-1. The survey consists of four main subfields, which include two non-contiguous fields at high Galactic latitudes (vertical bar b vertical bar > 30 degrees, 8000 deg(2)) and two areas of the Galactic Disc and Bulge (for an additional 1300 deg(2)). S-PLUS uses the Javalambre 12-band magnitude system, which includes the 5 ugriz broad-band filters and 7 narrow-band filters centred on prominent stellar spectral features: the Balmer jump/[OII], Ca H + K, Hd, G band, Mg b triplet, H alpha, and the Ca triplet. S-PLUS delivers accurate photometric redshifts (dz /(1 + z) = 0.02 or better) for galaxies with r < 19.7 AB mag and z < 0.4, thus producing a 3D map of the local Universe over a volume of more than 1 (Gpc/h)(3). The final S-PLUS catalogue will also enable the study of star formation and stellar populations in and around the Milky Way and nearby galaxies, as well as searches for quasars, variable sources, and low-metallicity stars. In this paper we introduce the main characteristics of the survey, illustrated with science verification data highlighting the unique capabilities of S-PLUS. We also present the first public data release of similar to 336 deg(2) of the Stripe 82 area, in 12 bands, to a limiting magnitude of r = 21, available at datalab.noao.edu/splus.© 2019 The Author(s).Published by Oxford University Press on behalf of the Royal Astronomical Society

Published
2019

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