scholarly journals AGE AND MASS CONSTRAINTS FOR A YOUNG MASSIVE CLUSTER IN M31 BASED ON SPECTRAL ENERGY DISTRIBUTION FITTING

2011 ◽  
Vol 141 (3) ◽  
pp. 86 ◽  
Author(s):  
Jun Ma ◽  
Song Wang ◽  
Zhenyu Wu ◽  
Zhou Fan ◽  
Yanbin Yang ◽  
...  
Keyword(s):  
Energy Distribution ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Distribution Fitting ◽  
Massive Cluster

scholarly journals Timing the earliest quenching events with a robust sample of massive quiescent galaxies at 2 < z < 5

2020 ◽  
Vol 496 (1) ◽  
pp. 695-707 ◽  
Author(s):  
A C Carnall ◽  
S Walker ◽  
R J McLure ◽  
J S Dunlop ◽  
D J McLeod ◽  
...  
Keyword(s):  
Energy Distribution ◽  
Selection Criteria ◽  
Spectral Energy Distribution ◽  
Photometric Data ◽  
Spectral Energy ◽  
Distribution Fitting ◽  
Star Forming ◽  
Photometric Redshift ◽  
The Times ◽  
Lower Redshift

ABSTRACT We present a sample of 151 massive (M* &gt; 1010 M⊙) quiescent galaxies at 2 &lt; z &lt; 5, based on a sophisticated Bayesian spectral energy distribution fitting analysis of the CANDELS UDS and GOODS-South fields. Our sample includes a robust sub-sample of 61 objects for which we confidently exclude low-redshift and star-forming solutions. We identify 10 robust objects at z &gt; 3, of which 2 are at z &gt; 4. We report formation redshifts, demonstrating that the oldest objects formed at z &gt; 6; however, individual ages from our photometric data have significant uncertainties, typically ∼0.5 Gyr. We demonstrate that the UVJ colours of the quiescent population evolve with redshift at z &gt; 3, becoming bluer and more similar to post-starburst galaxies at lower redshift. Based upon this, we construct a model for the time evolution of quiescent galaxy UVJ colours, concluding that the oldest objects are consistent with forming the bulk of their stellar mass at z ∼ 6–7 and quenching at z ∼ 5. We report spectroscopic redshifts for two of our objects at z = 3.440 and 3.396, which exhibit extremely weak Ly α emission in ultra-deep VANDELS spectra. We calculate star formation rates based on these line fluxes, finding that these galaxies are consistent with our quiescent selection criteria, provided their Ly α escape fractions are &gt;3 and &gt;10 per cent, respectively. We finally report that our highest redshift robust object exhibits a continuum break at λ ∼ 7000 Å in a spectrum from VUDS, consistent with our photometric redshift of $z_\mathrm{phot}=4.72^{+0.06}_{-0.04}$. If confirmed as quiescent, this object would be the highest redshift known quiescent galaxy. To obtain stronger constraints on the times of the earliest quenching events, high-SNR spectroscopy must be extended to z ≳ 3 quiescent objects.

scholarly journals SURVEY DESIGN FOR SPECTRAL ENERGY DISTRIBUTION FITTING: A FISHER MATRIX APPROACH

2012 ◽  
Vol 749 (1) ◽  
pp. 72 ◽  
Author(s):  
Viviana Acquaviva ◽  
Eric Gawiser ◽  
Steven J. Bickerton ◽  
Norman A. Grogin ◽  
Yicheng Guo ◽  
...  
Keyword(s):  
Energy Distribution ◽  
Survey Design ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Matrix Approach ◽  
Distribution Fitting ◽  
Fisher Matrix

scholarly journals DUST IN THE DIFFUSE EMISSION OF THE GALACTIC PLANE: THE HERSCHEL / SPITZER SPECTRAL ENERGY DISTRIBUTION FITTING

2010 ◽  
Vol 724 (1) ◽  
pp. L44-L47 ◽  
Author(s):  
M. Compiègne ◽  
N. Flagey ◽  
A. Noriega-Crespo ◽  
P. G. Martin ◽  
J.-P. Bernard ◽  
...  
Keyword(s):  
Energy Distribution ◽  
Galactic Plane ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Diffuse Emission ◽  
Distribution Fitting

scholarly journals MCSED: A Flexible Spectral Energy Distribution Fitting Code and Its Application to z ∼ 2 Emission-line Galaxies

2020 ◽  
Vol 899 (1) ◽  
pp. 7
Author(s):  
William P. Bowman ◽  
Gregory R. Zeimann ◽  
Gautam Nagaraj ◽  
Robin Ciardullo ◽  
Caryl Gronwall ◽  
...  
Keyword(s):  
Energy Distribution ◽  
Emission Line ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Distribution Fitting ◽  
Emission Line Galaxies

scholarly journals 3D Studies of Galaxies in Compact Groups

2014 ◽  
Vol 10 (S309) ◽  
pp. 175-177
Author(s):  
Claudia Mendes de Oliveira ◽  
Sergio Torres-Flores ◽  
Philippe Amram ◽  
Henri Plana ◽  
Benoit Epinat
Keyword(s):  
Star Formation ◽  
Energy Distribution ◽  
Compact Group ◽  
Spectral Energy Distribution ◽  
Interacting Galaxies ◽  
Spectral Energy ◽  
Compact Groups ◽  
Distribution Fitting ◽  
Fabry Perot ◽  
Fisher Relation

AbstractFabry-Perot data of compact group galaxies have been used to show that the Tully-Fisher relation in any photometric band, for galaxies with vmax > 100 km/s, is very similar to that for galaxies in other less dense environments. In the low-luminosity end, however, a few compact group galaxies fall above the relation apparently because they are too bright for their mass. Here we show that if the mass is properly computed from spectral energy distribution fitting or mass modelling, for the low-luminosity galaxies, their positions in the stellar-mass or baryonic Tully-Fisher relation are what is expected for a normal Tully-Fisher relation and the outlying positions observed in the B and K Tully-Fisher relation could be explained by brightening of the low-luminosity interacting galaxies due to strong star formation or AGN activity.

scholarly journals The Kinematics of Globular Cluster NGC 288

2001 ◽  
Vol 183 ◽  
pp. 333-334
Author(s):  
Chan-Kao Chang ◽  
Alfred B. Chen ◽  
Wean-Shun Tsay ◽  
Wen-Ping Chen ◽  
Phillip K. Lu
Keyword(s):  
Energy Distribution ◽  
Globular Cluster ◽  
Effective Temperature ◽  
Proper Motion ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Galactic Rotation ◽  
Distribution Fitting ◽  
The Mean ◽  
Effective Temperatures

AbstractThe mean radial velocity of NGC 288 (accuracy 5.5 km/s) is determined to be −56.3 ± 20.1 km/s which, when combined with the mean proper motion (Guo, 1995), yields a peculiar velocity with respect to the LSR of (u,v,w) = (29.7 ± 18.1, −258.6 ± 18.3,62.3 ± 20.3) km/s. This implies that NGC 288 moves in a retrograde sense with the Galactic rotation. We also derived the effective temperatures for stars in our sample and, as a corroborative effort, compared with those estimated previously from the BATC data (Tsai 1998) by spectral energy distribution fitting. We demonstrate that the BATC/SED fitting is an appropriate and efficient way to estimate the effective temperature of a star.

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