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Must Star-forming Galaxies Rapidly Get Denser before They Quench?
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| Zeitschriftentitel: | The Astrophysical Journal |
|---|---|
| Personen und Körperschaften: | , |
| In: | The Astrophysical Journal, 858, 2018, 1, S. 40 |
| Format: | E-Article |
| Sprache: | Unbestimmt |
| veröffentlicht: |
American Astronomical Society
|
| Schlagwörter: |
| author_facet |
Abramson, L. E. Morishita, T. Abramson, L. E. Morishita, T. |
|---|---|
| author |
Abramson, L. E. Morishita, T. |
| spellingShingle |
Abramson, L. E. Morishita, T. The Astrophysical Journal Must Star-forming Galaxies Rapidly Get Denser before They Quench? Space and Planetary Science Astronomy and Astrophysics |
| author_sort |
abramson, l. e. |
| spelling |
Abramson, L. E. Morishita, T. 0004-637X 1538-4357 American Astronomical Society Space and Planetary Science Astronomy and Astrophysics http://dx.doi.org/10.3847/1538-4357/aab61b <jats:title>Abstract</jats:title> <jats:p>Using the deepest data yet obtained, we find no evidence preferring compaction-triggered quenching—where rapid increases in galaxy density truncate star formation—over a null hypothesis in which galaxies age at constant surface density (<jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}\equiv {M}_{* }/2\pi {r}_{e}^{2}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn1.gif" xlink:type="simple" /> </jats:inline-formula>). Results from two fully empirical analyses and one quenching-free model calculation support this claim at all <jats:italic>z</jats:italic> ≤ 3: (1) qualitatively, galaxies’ mean <jats:italic>U</jats:italic>–<jats:italic>V</jats:italic> colors at <jats:inline-formula> <jats:tex-math> <?CDATA $6.5\,\lesssim \mathrm{log}{{\rm{\Sigma }}}_{e}/{\text{}}{M}_{\odot }\,{\mathrm{kpc}}^{-2}\lesssim 10$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn2.gif" xlink:type="simple" /> </jats:inline-formula> have reddened at rates/times correlated with <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn3.gif" xlink:type="simple" /> </jats:inline-formula>, implying that there is no density threshold at which galaxies turn red but that <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn4.gif" xlink:type="simple" /> </jats:inline-formula> sets the pace of maturation; (2) quantitatively, the abundance of <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{log}{M}_{* }/{\text{}}{M}_{\odot }\geqslant 9.4$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn5.gif" xlink:type="simple" /> </jats:inline-formula> red galaxies never exceeds that of the total population a quenching time earlier at any <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn6.gif" xlink:type="simple" /> </jats:inline-formula>, implying that galaxies need not transit from low to high densities before quenching; (3) applying <jats:inline-formula> <jats:tex-math> <?CDATA $d\mathrm{log}{r}_{e}/{dt}=1/2\,d\mathrm{log}{M}_{* }/{dt}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn7.gif" xlink:type="simple" /> </jats:inline-formula> to a suite of lognormal star formation histories reproduces the evolution of the size–mass relation at <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{log}{M}_{* }/{\text{}}{M}_{\odot }\geqslant 10$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn8.gif" xlink:type="simple" /> </jats:inline-formula>. All results are consistent with evolutionary rates being set ab initio by global densities, with denser objects evolving faster than less-dense ones toward a terminal quiescence induced by gas depletion or other ∼Hubble-timescale phenomena. Unless stellar ages demand otherwise, observed <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn9.gif" xlink:type="simple" /> </jats:inline-formula> thresholds need not bear any physical relation to quenching beyond this intrinsic density–formation epoch correlation, adding to Lilly & Carollo’s arguments to that effect.</jats:p> Must Star-forming Galaxies Rapidly Get Denser before They Quench? The Astrophysical Journal |
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10.3847/1538-4357/aab61b |
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American Astronomical Society, 2018 |
| imprint_str_mv |
American Astronomical Society, 2018 |
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0004-637X 1538-4357 |
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0004-637X 1538-4357 |
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Undetermined |
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American Astronomical Society (CrossRef) |
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abramson2018muststarforminggalaxiesrapidlygetdenserbeforetheyquench |
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2018 |
| publisher |
American Astronomical Society |
| recordtype |
ai |
| record_format |
ai |
| series |
The Astrophysical Journal |
| source_id |
49 |
| title |
Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_unstemmed |
Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_full |
Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_fullStr |
Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_full_unstemmed |
Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_short |
Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_sort |
must star-forming galaxies rapidly get denser before they quench? |
| topic |
Space and Planetary Science Astronomy and Astrophysics |
| url |
http://dx.doi.org/10.3847/1538-4357/aab61b |
| publishDate |
2018 |
| physical |
40 |
| description |
<jats:title>Abstract</jats:title>
<jats:p>Using the deepest data yet obtained, we find no evidence preferring compaction-triggered quenching—where rapid increases in galaxy density truncate star formation—over a null hypothesis in which galaxies age at constant surface density (<jats:inline-formula>
<jats:tex-math>
<?CDATA ${{\rm{\Sigma }}}_{e}\equiv {M}_{* }/2\pi {r}_{e}^{2}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn1.gif" xlink:type="simple" />
</jats:inline-formula>). Results from two fully empirical analyses and one quenching-free model calculation support this claim at all <jats:italic>z</jats:italic> ≤ 3: (1) qualitatively, galaxies’ mean <jats:italic>U</jats:italic>–<jats:italic>V</jats:italic> colors at <jats:inline-formula>
<jats:tex-math>
<?CDATA $6.5\,\lesssim \mathrm{log}{{\rm{\Sigma }}}_{e}/{\text{}}{M}_{\odot }\,{\mathrm{kpc}}^{-2}\lesssim 10$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn2.gif" xlink:type="simple" />
</jats:inline-formula> have reddened at rates/times correlated with <jats:inline-formula>
<jats:tex-math>
<?CDATA ${{\rm{\Sigma }}}_{e}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn3.gif" xlink:type="simple" />
</jats:inline-formula>, implying that there is no density threshold at which galaxies turn red but that <jats:inline-formula>
<jats:tex-math>
<?CDATA ${{\rm{\Sigma }}}_{e}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn4.gif" xlink:type="simple" />
</jats:inline-formula> sets the pace of maturation; (2) quantitatively, the abundance of <jats:inline-formula>
<jats:tex-math>
<?CDATA $\mathrm{log}{M}_{* }/{\text{}}{M}_{\odot }\geqslant 9.4$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn5.gif" xlink:type="simple" />
</jats:inline-formula> red galaxies never exceeds that of the total population a quenching time earlier at any <jats:inline-formula>
<jats:tex-math>
<?CDATA ${{\rm{\Sigma }}}_{e}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn6.gif" xlink:type="simple" />
</jats:inline-formula>, implying that galaxies need not transit from low to high densities before quenching; (3) applying <jats:inline-formula>
<jats:tex-math>
<?CDATA $d\mathrm{log}{r}_{e}/{dt}=1/2\,d\mathrm{log}{M}_{* }/{dt}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn7.gif" xlink:type="simple" />
</jats:inline-formula> to a suite of lognormal star formation histories reproduces the evolution of the size–mass relation at <jats:inline-formula>
<jats:tex-math>
<?CDATA $\mathrm{log}{M}_{* }/{\text{}}{M}_{\odot }\geqslant 10$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn8.gif" xlink:type="simple" />
</jats:inline-formula>. All results are consistent with evolutionary rates being set ab initio by global densities, with denser objects evolving faster than less-dense ones toward a terminal quiescence induced by gas depletion or other ∼Hubble-timescale phenomena. Unless stellar ages demand otherwise, observed <jats:inline-formula>
<jats:tex-math>
<?CDATA ${{\rm{\Sigma }}}_{e}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn9.gif" xlink:type="simple" />
</jats:inline-formula> thresholds need not bear any physical relation to quenching beyond this intrinsic density–formation epoch correlation, adding to Lilly & Carollo’s arguments to that effect.</jats:p> |
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| description | <jats:title>Abstract</jats:title> <jats:p>Using the deepest data yet obtained, we find no evidence preferring compaction-triggered quenching—where rapid increases in galaxy density truncate star formation—over a null hypothesis in which galaxies age at constant surface density (<jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}\equiv {M}_{* }/2\pi {r}_{e}^{2}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn1.gif" xlink:type="simple" /> </jats:inline-formula>). Results from two fully empirical analyses and one quenching-free model calculation support this claim at all <jats:italic>z</jats:italic> ≤ 3: (1) qualitatively, galaxies’ mean <jats:italic>U</jats:italic>–<jats:italic>V</jats:italic> colors at <jats:inline-formula> <jats:tex-math> <?CDATA $6.5\,\lesssim \mathrm{log}{{\rm{\Sigma }}}_{e}/{\text{}}{M}_{\odot }\,{\mathrm{kpc}}^{-2}\lesssim 10$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn2.gif" xlink:type="simple" /> </jats:inline-formula> have reddened at rates/times correlated with <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn3.gif" xlink:type="simple" /> </jats:inline-formula>, implying that there is no density threshold at which galaxies turn red but that <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn4.gif" xlink:type="simple" /> </jats:inline-formula> sets the pace of maturation; (2) quantitatively, the abundance of <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{log}{M}_{* }/{\text{}}{M}_{\odot }\geqslant 9.4$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn5.gif" xlink:type="simple" /> </jats:inline-formula> red galaxies never exceeds that of the total population a quenching time earlier at any <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn6.gif" xlink:type="simple" /> </jats:inline-formula>, implying that galaxies need not transit from low to high densities before quenching; (3) applying <jats:inline-formula> <jats:tex-math> <?CDATA $d\mathrm{log}{r}_{e}/{dt}=1/2\,d\mathrm{log}{M}_{* }/{dt}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn7.gif" xlink:type="simple" /> </jats:inline-formula> to a suite of lognormal star formation histories reproduces the evolution of the size–mass relation at <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{log}{M}_{* }/{\text{}}{M}_{\odot }\geqslant 10$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn8.gif" xlink:type="simple" /> </jats:inline-formula>. All results are consistent with evolutionary rates being set ab initio by global densities, with denser objects evolving faster than less-dense ones toward a terminal quiescence induced by gas depletion or other ∼Hubble-timescale phenomena. Unless stellar ages demand otherwise, observed <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn9.gif" xlink:type="simple" /> </jats:inline-formula> thresholds need not bear any physical relation to quenching beyond this intrinsic density–formation epoch correlation, adding to Lilly & Carollo’s arguments to that effect.</jats:p> |
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| id | ai-49-aHR0cDovL2R4LmRvaS5vcmcvMTAuMzg0Ny8xNTM4LTQzNTcvYWFiNjFi |
| imprint | American Astronomical Society, 2018 |
| imprint_str_mv | American Astronomical Society, 2018 |
| institution | DE-D275, DE-Bn3, DE-Brt1, DE-D161, DE-Zwi2, DE-Gla1, DE-Zi4, DE-15, DE-Pl11, DE-Rs1, DE-105, DE-14, DE-Ch1, DE-L229 |
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| last_indexed | 2024-03-01T16:40:32.731Z |
| match_str | abramson2018muststarforminggalaxiesrapidlygetdenserbeforetheyquench |
| mega_collection | American Astronomical Society (CrossRef) |
| physical | 40 |
| publishDate | 2018 |
| publishDateSort | 2018 |
| publisher | American Astronomical Society |
| record_format | ai |
| recordtype | ai |
| series | The Astrophysical Journal |
| source_id | 49 |
| spelling | Abramson, L. E. Morishita, T. 0004-637X 1538-4357 American Astronomical Society Space and Planetary Science Astronomy and Astrophysics http://dx.doi.org/10.3847/1538-4357/aab61b <jats:title>Abstract</jats:title> <jats:p>Using the deepest data yet obtained, we find no evidence preferring compaction-triggered quenching—where rapid increases in galaxy density truncate star formation—over a null hypothesis in which galaxies age at constant surface density (<jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}\equiv {M}_{* }/2\pi {r}_{e}^{2}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn1.gif" xlink:type="simple" /> </jats:inline-formula>). Results from two fully empirical analyses and one quenching-free model calculation support this claim at all <jats:italic>z</jats:italic> ≤ 3: (1) qualitatively, galaxies’ mean <jats:italic>U</jats:italic>–<jats:italic>V</jats:italic> colors at <jats:inline-formula> <jats:tex-math> <?CDATA $6.5\,\lesssim \mathrm{log}{{\rm{\Sigma }}}_{e}/{\text{}}{M}_{\odot }\,{\mathrm{kpc}}^{-2}\lesssim 10$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn2.gif" xlink:type="simple" /> </jats:inline-formula> have reddened at rates/times correlated with <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn3.gif" xlink:type="simple" /> </jats:inline-formula>, implying that there is no density threshold at which galaxies turn red but that <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn4.gif" xlink:type="simple" /> </jats:inline-formula> sets the pace of maturation; (2) quantitatively, the abundance of <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{log}{M}_{* }/{\text{}}{M}_{\odot }\geqslant 9.4$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn5.gif" xlink:type="simple" /> </jats:inline-formula> red galaxies never exceeds that of the total population a quenching time earlier at any <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn6.gif" xlink:type="simple" /> </jats:inline-formula>, implying that galaxies need not transit from low to high densities before quenching; (3) applying <jats:inline-formula> <jats:tex-math> <?CDATA $d\mathrm{log}{r}_{e}/{dt}=1/2\,d\mathrm{log}{M}_{* }/{dt}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn7.gif" xlink:type="simple" /> </jats:inline-formula> to a suite of lognormal star formation histories reproduces the evolution of the size–mass relation at <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{log}{M}_{* }/{\text{}}{M}_{\odot }\geqslant 10$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn8.gif" xlink:type="simple" /> </jats:inline-formula>. All results are consistent with evolutionary rates being set ab initio by global densities, with denser objects evolving faster than less-dense ones toward a terminal quiescence induced by gas depletion or other ∼Hubble-timescale phenomena. Unless stellar ages demand otherwise, observed <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Sigma }}}_{e}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaab61bieqn9.gif" xlink:type="simple" /> </jats:inline-formula> thresholds need not bear any physical relation to quenching beyond this intrinsic density–formation epoch correlation, adding to Lilly & Carollo’s arguments to that effect.</jats:p> Must Star-forming Galaxies Rapidly Get Denser before They Quench? The Astrophysical Journal |
| spellingShingle | Abramson, L. E., Morishita, T., The Astrophysical Journal, Must Star-forming Galaxies Rapidly Get Denser before They Quench?, Space and Planetary Science, Astronomy and Astrophysics |
| title | Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_full | Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_fullStr | Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_full_unstemmed | Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_short | Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| title_sort | must star-forming galaxies rapidly get denser before they quench? |
| title_unstemmed | Must Star-forming Galaxies Rapidly Get Denser before They Quench? |
| topic | Space and Planetary Science, Astronomy and Astrophysics |
| url | http://dx.doi.org/10.3847/1538-4357/aab61b |