scholarly journals Cosmic Star Formation History Revealed by the Akari & Spatially-Resolved Spectroscopy of an E+A (Post-Starburst) System

2010 ◽  
Author(s):  
Tomotsugu Goto ◽  
M. Yagi ◽  
C. Yamauchi ◽  
Victor P. Debattista ◽  
C. C. Popescu ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation History ◽  
Spatially Resolved ◽  
Formation History ◽  
Spatially Resolved Spectroscopy

scholarly journals Spatially resolved LMC star formation history – I. Outside in evolution of the outer LMC disc

2013 ◽  
Vol 438 (2) ◽  
pp. 1067-1080 ◽  
Author(s):  
I. Meschin ◽  
C. Gallart ◽  
A. Aparicio ◽  
S. L. Hidalgo ◽  
M. Monelli ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation History ◽  
Spatially Resolved ◽  
Formation History

scholarly journals On the Spatially Resolved Star Formation History in M51. I. Hybrid UV+IR Star Formation Laws and IR Emission from Dust Heated by Old Stars

2017 ◽  
Vol 851 (1) ◽  
pp. 10 ◽  
Author(s):  
R. T. Eufrasio ◽  
B. D. Lehmer ◽  
A. Zezas ◽  
E. Dwek ◽  
R. G. Arendt ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation History ◽  
Spatially Resolved ◽  
Formation History ◽  
Ir Emission

scholarly journals The spatially resolved star formation history of mergers

2017 ◽  
Vol 607 ◽  
pp. A70 ◽  
Author(s):  
C. Cortijo-Ferrero ◽  
R. M. González Delgado ◽  
E. Pérez ◽  
R. Cid Fernandes ◽  
R. García-Benito ◽  
...  
Keyword(s):  
Star Formation ◽  
Time Scales ◽  
Time Scale ◽  
Star Formation Rate ◽  
Early Stage ◽  
Formation Rate ◽  
Small Sample ◽  
Star Formation History ◽  
Spatially Resolved ◽  
Formation History

This paper presents the spatially resolved star formation history (2D-SFH) of a small sample of four local mergers: the early-stage mergers IC 1623, NGC 6090, and the Mice, and the more advanced merger NGC 2623, by analyzing IFS data from the CALIFA survey and PMAS in LArr mode. Full spectral fitting techniques are applied to the datacubes to obtain the spatially resolved mass growth histories, the time evolution of the star formation rate intensity (ΣSFR), and the local specific star formation rate (sSFR), over three different time scales (30 Myr, 300 Myr, and 1 Gyr). The results are compared with non-interacting Sbc–Sc galaxies, to quantify if there is an enhancement of the star formation and to trace its time scale and spatial extent. Our results for the three LIRGs (IC 1623 W, NGC 6090, and NGC 2623) show that a major phase of star formation is occurring in time scales of 107 yr to few 108 yr, with global SFR enhancements of between approximately two and six with respect to main-sequence star forming (MSSF) galaxies. In the two early-stage mergers IC 1623 W and NGC 6090, which are between first pericentre passage and coalescence, the most remarkable increase of the SFR with respect to non-interacting spirals occurred in the last 30 Myr, and it is spatially extended, with enhancements of factors between two and seven both in the centres (r < 0.5 half light radius, HLR), and in the disks (r > 1 HLR). In the more advanced merger NGC 2623 an extended phase of star formation occurred on a longer time scale of ~1 Gyr, with a SFR enhancement of a factor of approximately two-to-three larger than the one in Sbc–Sc MSSF galaxies over the same period, probably relic of the first pericentre passage epoch. A SFR enhancement in the last 30 Myr is also present, but only in NGC 2623 centre, by a factor of three. In general, the spatially resolved SFHs of the LIRG-mergers are consistent with the predictions from high spatial resolution simulations. In contrast, the star formation in the Mice, specially in Mice B, is not enhanced but inhibited with respect to Sbc–Sc MSSF galaxies. The fact that the gas fraction of Mice B is smaller than in most non-interacting spirals, and that the Mice are close to a prograde orbit, represents a new challenge for the models, which must cover a larger space of parameters in terms of the availability of gas and the orbital characteristics.

scholarly journals Deep [ITAL]Hubble Space Telescope[/ITAL] Imaging of Sextans A. I. The Spatially Resolved Recent Star Formation History

2002 ◽  
Vol 123 (2) ◽  
pp. 813-831 ◽  
Author(s):  
Robbie C. Dohm-Palmer ◽  
Evan D. Skillman ◽  
Mario Mateo ◽  
Abi Saha ◽  
Andrew Dolphin ◽  
...  
Keyword(s):  
Star Formation ◽  
Hubble Space Telescope ◽  
Star Formation History ◽  
Space Telescope ◽  
Spatially Resolved ◽  
Formation History

scholarly journals Spatially Resolved Stellar Spectroscopy of the Ultra-diffuse Galaxy Dragonfly 44. III. Evidence for an Unexpected Star Formation History under Conventional Galaxy Evolution Processes

2022 ◽  
Vol 924 (1) ◽  
pp. 32
Author(s):  
Alexa Villaume ◽  
Aaron J. Romanowsky ◽  
Jean Brodie ◽  
Pieter van Dokkum ◽  
Charlie Conroy ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Globular Clusters ◽  
Stellar Population ◽  
Dwarf Galaxies ◽  
Star Formation History ◽  
Population Parameters ◽  
Spatially Resolved ◽  
Formation History ◽  
Field Unit

Abstract We use the Keck Cosmic Web Imager integral field unit spectrograph to (1) measure the global stellar population parameters for the ultra-diffuse galaxy (UDG) Dragonfly 44 (DF44) to much higher precision than previously possible for any UDG and (2) for the first time measure spatially resolved stellar population parameters of a UDG. We find that DF44 falls below the mass–metallicity relation established by canonical dwarf galaxies both in and beyond the Local Group. We measure a flat radial age gradient ( m logage = + 0.01 − 0.08 + 0.08 log Gyr kpc−1) and a flat to positive metallicity gradient ( m [ Fe / H ] = + 0.09 − 0.12 + 0.11 dex kpc−1), which are inconsistent with the gradients measured in similarly pressure-supported dwarf galaxies. We also measure a negative [Mg/Fe] gradient ( m [ Mg / Fe ] = − 0.20 − 0.18 + 0.18 ) dex kpc−1 such that the central 1.5 kpc of DF44 has stellar population parameters comparable to metal-poor globular clusters. Overall, DF44 does not have internal properties similar to other dwarf galaxies and is inconsistent with it having been puffed up through a prolonged, bursty star formation history, as suggested by some simulations. Rather, the evidence indicates that DF44 experienced an intense epoch of “inside-out” star formation and then quenched early and catastrophically, such that star formation was cut off more quickly than in canonical dwarf galaxies.

scholarly journals THE PANCHROMATICHUBBLEANDROMEDA TREASURY. XI. THE SPATIALLY RESOLVED RECENT STAR FORMATION HISTORY OF M31

2015 ◽  
Vol 805 (2) ◽  
pp. 183 ◽  
Author(s):  
Alexia R. Lewis ◽  
Andrew E. Dolphin ◽  
Julianne J. Dalcanton ◽  
Daniel R. Weisz ◽  
Benjamin F. Williams ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation History ◽  
Spatially Resolved ◽  
Formation History ◽  
History Of

scholarly journals Reconstructing the Star Formation History of the Magellanic Clouds

1999 ◽  
Vol 192 ◽  
pp. 72-78
Author(s):  
Jason Harris ◽  
Dennis Zaritsky ◽  
Eva K. Grebel ◽  
Ian Thompson
Keyword(s):  
Star Formation ◽  
Stellar Population ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Photometric Data ◽  
Star Formation History ◽  
Spatially Resolved ◽  
Formation History ◽  
History Of

We are developing an algorithm to determine the star formation history (SFH) of a mixed stellar population. We will apply the algorithm to hundreds of regions in our Magellanic Clouds Photometric Survey data and reconstruct the spatially resolved star formation history of the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC). In this paper, we demonstrate the algorithm on a typical region in the LMC, focussing on the obstacles and challenges facing us in attempting to reliably extract the SFH from photometric data.

scholarly journals A MEGACAM SURVEY OF OUTER HALO SATELLITES. VI. THE SPATIALLY RESOLVED STAR-FORMATION HISTORY OF THE CARINA DWARF SPHEROIDAL GALAXY

2016 ◽  
Vol 829 (2) ◽  
pp. 86 ◽  
Author(s):  
Felipe A. Santana ◽  
Ricardo R. Muñoz ◽  
T. J. L. de Boer ◽  
Joshua D. Simon ◽  
Marla Geha ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation History ◽  
Spatially Resolved ◽  
Formation History ◽  
History Of
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