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1. Candidate Massive Galaxies at $z \sim 4$ in the Dark Energy Survey

Author

Guarnieri, Pierandrea, Maraston, Claudia, Thomas, Daniel, Pforr, Janine, Gonzalez-Perez, Violeta, Etherington, James, Carlsen, Joakim, Morice-Atkinson, Xan, Conselice, Christopher J., Gschwend, Julia, Kind, Matias Carrasco, Abbott, Tim, Allam, Sahar, Brooks, David, Burke, David, Rosell, Aurelio Carnero, Carretero, Jorge, Cunha, Carlos, ďAndrea, Chris, da Costa, Luiz, De Vincente, Juan, DePoy, Darren, Diehl, H. Thomas, Doel, Peter, Frieman, Josh, Garcia-Bellido, Juan, Gruen, Daniel, Gutierrez, Gaston, Hanley, Dominic, Hollowood, Devon, Honscheid, Klaus, James, David, Jeltema, Tesla, Kuehn, Kyler, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer, Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Malagon, Andres Plazas, Richardson, Samuel, Romer, Kathy, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Sevilla, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Tarle, Gregory, Walker, Alistair, and Wester, William

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Using stellar population models, we predicted that the Dark Energy Survey (DES) - due to its special combination of area (5000 deg. sq.) and depth ($i = 24.3$) - would be in the position to detect massive ($\gtrsim 10^{11}$ M$_{\odot}$) galaxies at $z \sim 4$. We confront those theoretical calculations with the first $\sim 150$ deg. sq. of DES data reaching nominal depth. From a catalogue containing $\sim 5$ million sources, $\sim26000$ were found to have observed-frame $g-r$ vs $r-i$ colours within the locus predicted for $z \sim 4$ massive galaxies. We further removed contamination by stars and artefacts, obtaining 606 galaxies lining up by the model selection box. We obtained their photometric redshifts and physical properties by fitting model templates spanning a wide range of star formation histories, reddening and redshift. Key to constrain the models is the addition, to the optical DES bands $g$, $r$, $i$, $z$, and $Y$, of near-IR $J$, $H$, $K_{s}$ data from the Vista Hemisphere Survey. We further applied several quality cuts to the fitting results, including goodness of fit and a unimodal redshift probability distribution. We finally select 233 candidates whose photometric redshift probability distribution function peaks around $z\sim4$, have high stellar masses ($\log($M$^{*}$/M$_{\odot})\sim 11.7$ for a Salpeter IMF) and ages around 0.1 Gyr, i.e. formation redshift around 5. These properties match those of the progenitors of the most massive galaxies in the local universe. This is an ideal sample for spectroscopic follow-up to select the fraction of galaxies which is truly at high redshift. These initial results and those at the survey completion, which we shall push to higher redshifts, will set unprecedented constraints on galaxy formation, evolution, and the re-ionisation epoch., Comment: 24 pages (41 with appendix), 16 figures, MNRAS in press

Published
2018
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2. Candidate Massive Galaxies at z~4 in the Dark Energy Survey

Author

Guarnieri, Pierandrea, Maraston, Claudia, Thomas, Daniel, Pforr, Janine, Gonzalez-Perez, Violeta, Etherington, James, Carlsen, Joakim, Morice-Atkinson, Xan, Conselice, Christopher J., Gschwend, Julia, Kind, Matias Carrasco, Abbott, Tim, Allam, Sahar, Brooks, David, Burke, David, Rosell, Aurelio Carnero, Carretero, Jorge, Cunha, Carlos, ďAndrea, Chris, Costa, Luiz da, Vincente, Juan De, DePoy, Darren, Diehl, H. Thomas, Doel, Peter, Frieman, Josh, Garcia-Bellido, Juan, Gruen, Daniel, Gutierrez, Gaston, Hanley, Dominic, Hollowood, Devon, Honscheid, Klaus, James, David, Jeltema, Tesla, Kuehn, Kyler, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer, Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Malagon, Andres Plazas, Richardson, Samuel, Romer, Kathy, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Sevilla, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Tarle, Gregory, Walker, Alistair, Wester, William, Guarnieri, Pierandrea, Maraston, Claudia, Thomas, Daniel, Pforr, Janine, Gonzalez-Perez, Violeta, Etherington, James, Carlsen, Joakim, Morice-Atkinson, Xan, Conselice, Christopher J., Gschwend, Julia, Kind, Matias Carrasco, Abbott, Tim, Allam, Sahar, Brooks, David, Burke, David, Rosell, Aurelio Carnero, Carretero, Jorge, Cunha, Carlos, ďAndrea, Chris, Costa, Luiz da, Vincente, Juan De, DePoy, Darren, Diehl, H. Thomas, Doel, Peter, Frieman, Josh, Garcia-Bellido, Juan, Gruen, Daniel, Gutierrez, Gaston, Hanley, Dominic, Hollowood, Devon, Honscheid, Klaus, James, David, Jeltema, Tesla, Kuehn, Kyler, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer, Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Malagon, Andres Plazas, Richardson, Samuel, Romer, Kathy, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Sevilla, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Tarle, Gregory, Walker, Alistair, and Wester, William

Abstract

Using stellar population models, we predicted that the Dark Energy Survey (DES) - due to its special combination of area (5000 deg. sq.) and depth ($i = 24.3$) - would be in the position to detect massive ($\gtrsim 10^{11}$ M$_{\odot}$) galaxies at $z \sim 4$. We confront those theoretical calculations with the first $\sim 150$ deg. sq. of DES data reaching nominal depth. From a catalogue containing $\sim 5$ million sources, $\sim26000$ were found to have observed-frame $g-r$ vs $r-i$ colours within the locus predicted for $z \sim 4$ massive galaxies. We further removed contamination by stars and artefacts, obtaining 606 galaxies lining up by the model selection box. We obtained their photometric redshifts and physical properties by fitting model templates spanning a wide range of star formation histories, reddening and redshift. Key to constrain the models is the addition, to the optical DES bands $g$, $r$, $i$, $z$, and $Y$, of near-IR $J$, $H$, $K_{s}$ data from the Vista Hemisphere Survey. We further applied several quality cuts to the fitting results, including goodness of fit and a unimodal redshift probability distribution. We finally select 233 candidates whose photometric redshift probability distribution function peaks around $z\sim4$, have high stellar masses ($\log($M$^{*}$/M$_{\odot})\sim 11.7$ for a Salpeter IMF) and ages around 0.1 Gyr, i.e. formation redshift around 5. These properties match those of the progenitors of the most massive galaxies in the local universe. This is an ideal sample for spectroscopic follow-up to select the fraction of galaxies which is truly at high redshift. These initial results and those at the survey completion, which we shall push to higher redshifts, will set unprecedented constraints on galaxy formation, evolution, and the re-ionisation epoch.

Published
2019

3. Candidate massive galaxies atz ∼ 4 in the Dark Energy Survey

Author

Guarnieri, Pierandrea, primary, Maraston, Claudia, additional, Thomas, Daniel, additional, Pforr, Janine, additional, Gonzalez-Perez, Violeta, additional, Etherington, James, additional, Carlsen, Joakim, additional, Morice-Atkinson, Xan, additional, Conselice, Christopher J, additional, Gschwend, Julia, additional, Carrasco Kind, Matias, additional, Abbott, Tim, additional, Allam, Sahar, additional, Brooks, David, additional, Burke, David, additional, Carnero Rosell, Aurelio, additional, Carretero, Jorge, additional, Cunha, Carlos, additional, D’Andrea, Chris, additional, da Costa, Luiz, additional, De Vincente, Juan, additional, DePoy, Darren, additional, Thomas Diehl, H, additional, Doel, Peter, additional, Frieman, Josh, additional, Garcia-Bellido, Juan, additional, Gruen, Daniel, additional, Gutierrez, Gaston, additional, Hanley, Dominic, additional, Hollowood, Devon, additional, Honscheid, Klaus, additional, James, David, additional, Jeltema, Tesla, additional, Kuehn, Kyler, additional, Lima, Marcos, additional, Maia, Marcio A G, additional, Marshall, Jennifer, additional, Martini, Paul, additional, Melchior, Peter, additional, Menanteau, Felipe, additional, Miquel, Ramon, additional, Plazas Malagon, Andres, additional, Richardson, Samuel, additional, Romer, Kathy, additional, Sanchez, Eusebio, additional, Scarpine, Vic, additional, Schindler, Rafe, additional, Sevilla, Ignacio, additional, Smith, Mathew, additional, Soares-Santos, Marcelle, additional, Sobreira, Flavia, additional, Suchyta, Eric, additional, Tarle, Gregory, additional, Walker, Alistair, additional, and Wester, William, additional

Published
2018
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4. Effekten av spenst- og hurtighetstrening på hurtighet hos unge fotballspillere

Author

Carlsen, Joakim Strand, Fadnes, Kristoffer, and Karlsen, Kjell Anders Furulund

Subjects
hurtighetstrening, unge, fotball, spensttrening
Abstract

Formål med studiet: Undersøke effekten av spenst- og hurtighetstrening på hurtighet hos unge fotballspillere i sesong. Videre se på hvilken trening som var mest effektiv av spenst- og hurtighetstrening, og hvilken betydning dette evt. ville ha på fotballspillet. Metode: 30 mannlige unge fotballspillere født fra 1996 til 2002 fullførte en intervensjonsstudie bestående av spenst- eller hurtighetstrening. Deltagerne ble delt i to grupper, hurtighet og spenst. Hurtighetsgruppen løp 6 repetisjoner av 30 meter sprinter, mens spenstgruppen gjennomførte 3 sett bestående av 5 horisontale hopp over hekk. 2-3 ganger i uken i 6 uker som et supplement til vanlig trening. Begge gruppene hadde felles oppvarming bestående av 10 minutter jogging og 2 minutter pause mellom hvert sett. Alle deltagerne ble testet på 5 meter, 10 meter og 30 meter sprint både før og etter intervensjon. Resultater: Hurtighetsgruppen forbedret seg med 5,02 % på 5 meter, 2,19 % på 10 meter og 0,94 % på 30 meter fra pre- mot post test. Spenstgruppen forbedret seg 8,55 % på 5 meter, 4,53 % på 10 meter og 2,37 % på 30 meter. Konklusjon: Hovedfunnene i dette studiet viste at det ikke var signifikant forskjell i fremgang mellom de to treningsgruppene. Effekten av spensttreningen er like stor som effekten av hurtighetstreningen, samtidig som det tar kortere tid og mindre plass å gjennomføre spensttreningen. Det vil derfor være anbefalt å gjennomføre spensttreningen fremfor hurtighetstreningen.

Published
2016

5. Candidate massive galaxies at z  ∼ 4 in the Dark Energy Survey.

Author

Guarnieri, Pierandrea, Maraston, Claudia, Thomas, Daniel, Pforr, Janine, Gonzalez-Perez, Violeta, Etherington, James, Carlsen, Joakim, Morice-Atkinson, Xan, Conselice, Christopher J, Gschwend, Julia, Carrasco Kind, Matias, Abbott, Tim, Allam, Sahar, Brooks, David, Burke, David, Carnero Rosell, Aurelio, Carretero, Jorge, Cunha, Carlos, D'Andrea, Chris, and da Costa, Luiz

Subjects
DARK energy, STELLAR populations, GALAXIES, REDSHIFT, ASTRONOMICAL photometry
Abstract

Using stellar population models, we predicted that the Dark Energy Survey (DES) – due to its special combination of area (5000 deg2) and depth (i  = 24.3) – would be in the position to detect massive (≳1011 M⊙) galaxies at |$z$|  ∼ 4. We confront those theoretical calculations with the first ∼150 deg2 of DES data reaching nominal depth. From a catalogue containing ∼5 million sources, ∼26 000 were found to have observed-frame g − r versus  r − i colours within the locus predicted for |$z$|  ∼ 4 massive galaxies. We further removed contamination by stars and artefacts, obtaining 606 galaxies lining up by the model selection box. We obtained their photometric redshifts and physical properties by fitting model templates spanning a wide range of star formation histories, reddening and redshift. Key to constrain the models is the addition, to the optical DES bands g, r, i, |$z$|⁠, and Y, of near-IR J, H, Ks data from the Vista Hemisphere Survey. We further applied several quality cuts to the fitting results, including goodness of fit and a unimodal redshift probability distribution. We finally select 233 candidates whose photometric redshift probability distribution function peaks around |$z$|  ∼ 4, have high stellar masses [log (M */M⊙) ∼ 11.7 for a Salpeter IMF] and ages around 0.1 Gyr, i.e. formation redshift around 5. These properties match those of the progenitors of the most massive galaxies in the local Universe. This is an ideal sample for spectroscopic follow-up to select the fraction of galaxies which are truly at high redshift. These initial results and those at the survey completion, which we shall push to higher redshifts, will set unprecedented constraints on galaxy formation, evolution, and the re-ionization epoch. [ABSTRACT FROM AUTHOR]

Published
2019
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