No more active galactic nuclei in clumpy disks than in smooth galaxies at z ∼ 2 in candels/3D-HST

Jonathan R. Trump, Guillermo Barro, Stéphanie Juneau, Benjamin J. Weiner, Bin Luo, Gabriel B. Brammer, Eric F. Bell, W. N. Brandt, Avishai Dekel, Yicheng Guo, Philip F. Hopkins, David C. Koo, Dale D. Kocevski, Daniel H. McIntosh, Ivelina Momcheva, S. M. Faber, Henry C. Ferguson, Norman A. Grogin, Jeyhan Kartaltepe, Anton M. KoekemoerJennifer Lotz, Michael Maseda, Mark Mozena, Kirpal Nandra, David J. Rosario, Gregory R. Zeimann

Research output: Contribution to journalArticle

13 Citations (Scopus)

Abstract

We use CANDELS imaging, 3D-HST spectroscopy, and Chandra X-ray data to investigate if active galactic nuclei (AGNs) are preferentially fueled by violent disk instabilities funneling gas into galaxy centers at 1.3 < z < 2.4. We select galaxies undergoing gravitational instabilities using the number of clumps and degree of patchiness as proxies. The CANDELS visual classification system is used to identify 44 clumpy disk galaxies, along with mass-matched comparison samples of smooth and intermediate morphology galaxies. We note that despite being mass-matched and having similar star formation rates, the smoother galaxies tend to be smaller disks with more prominent bulges compared to the clumpy galaxies. The lack of smooth extended disks is probably a general feature of the z ∼ 2 galaxy population, and means we cannot directly compare with the clumpy and smooth extended disks observed at lower redshift. We find that z ∼ 2 clumpy galaxies have slightly enhanced AGN fractions selected by integrated line ratios (in the mass-excitation method), but the spatially resolved line ratios indicate this is likely due to extended phenomena rather than nuclear AGNs. Meanwhile, the X-ray data show that clumpy, smooth, and intermediate galaxies have nearly indistinguishable AGN fractions derived from both individual detections and stacked non-detections. The data demonstrate that AGN fueling modes at z ∼ 1.85 - whether violent disk instabilities or secular processes - are as efficient in smooth galaxies as they are in clumpy galaxies.

Original languageEnglish (US)
Article number101
JournalAstrophysical Journal
Volume793
Issue number2
DOIs
StatePublished - Oct 1 2014

Fingerprint

active galactic nuclei
galaxies
patchiness
spectroscopy
gas
gravitational instability
refueling
disk galaxies
clumps
star formation rate
x rays
gases
detection
rate
comparison
method

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Trump, J. R., Barro, G., Juneau, S., Weiner, B. J., Luo, B., Brammer, G. B., ... Zeimann, G. R. (2014). No more active galactic nuclei in clumpy disks than in smooth galaxies at z ∼ 2 in candels/3D-HST. Astrophysical Journal, 793(2), [101]. https://doi.org/10.1088/0004-637X/793/2/101
Trump, Jonathan R. ; Barro, Guillermo ; Juneau, Stéphanie ; Weiner, Benjamin J. ; Luo, Bin ; Brammer, Gabriel B. ; Bell, Eric F. ; Brandt, W. N. ; Dekel, Avishai ; Guo, Yicheng ; Hopkins, Philip F. ; Koo, David C. ; Kocevski, Dale D. ; McIntosh, Daniel H. ; Momcheva, Ivelina ; Faber, S. M. ; Ferguson, Henry C. ; Grogin, Norman A. ; Kartaltepe, Jeyhan ; Koekemoer, Anton M. ; Lotz, Jennifer ; Maseda, Michael ; Mozena, Mark ; Nandra, Kirpal ; Rosario, David J. ; Zeimann, Gregory R. / No more active galactic nuclei in clumpy disks than in smooth galaxies at z ∼ 2 in candels/3D-HST. In: Astrophysical Journal. 2014 ; Vol. 793, No. 2.
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abstract = "We use CANDELS imaging, 3D-HST spectroscopy, and Chandra X-ray data to investigate if active galactic nuclei (AGNs) are preferentially fueled by violent disk instabilities funneling gas into galaxy centers at 1.3 < z < 2.4. We select galaxies undergoing gravitational instabilities using the number of clumps and degree of patchiness as proxies. The CANDELS visual classification system is used to identify 44 clumpy disk galaxies, along with mass-matched comparison samples of smooth and intermediate morphology galaxies. We note that despite being mass-matched and having similar star formation rates, the smoother galaxies tend to be smaller disks with more prominent bulges compared to the clumpy galaxies. The lack of smooth extended disks is probably a general feature of the z ∼ 2 galaxy population, and means we cannot directly compare with the clumpy and smooth extended disks observed at lower redshift. We find that z ∼ 2 clumpy galaxies have slightly enhanced AGN fractions selected by integrated line ratios (in the mass-excitation method), but the spatially resolved line ratios indicate this is likely due to extended phenomena rather than nuclear AGNs. Meanwhile, the X-ray data show that clumpy, smooth, and intermediate galaxies have nearly indistinguishable AGN fractions derived from both individual detections and stacked non-detections. The data demonstrate that AGN fueling modes at z ∼ 1.85 - whether violent disk instabilities or secular processes - are as efficient in smooth galaxies as they are in clumpy galaxies.",
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Trump, JR, Barro, G, Juneau, S, Weiner, BJ, Luo, B, Brammer, GB, Bell, EF, Brandt, WN, Dekel, A, Guo, Y, Hopkins, PF, Koo, DC, Kocevski, DD, McIntosh, DH, Momcheva, I, Faber, SM, Ferguson, HC, Grogin, NA, Kartaltepe, J, Koekemoer, AM, Lotz, J, Maseda, M, Mozena, M, Nandra, K, Rosario, DJ & Zeimann, GR 2014, 'No more active galactic nuclei in clumpy disks than in smooth galaxies at z ∼ 2 in candels/3D-HST', Astrophysical Journal, vol. 793, no. 2, 101. https://doi.org/10.1088/0004-637X/793/2/101

No more active galactic nuclei in clumpy disks than in smooth galaxies at z ∼ 2 in candels/3D-HST. / Trump, Jonathan R.; Barro, Guillermo; Juneau, Stéphanie; Weiner, Benjamin J.; Luo, Bin; Brammer, Gabriel B.; Bell, Eric F.; Brandt, W. N.; Dekel, Avishai; Guo, Yicheng; Hopkins, Philip F.; Koo, David C.; Kocevski, Dale D.; McIntosh, Daniel H.; Momcheva, Ivelina; Faber, S. M.; Ferguson, Henry C.; Grogin, Norman A.; Kartaltepe, Jeyhan; Koekemoer, Anton M.; Lotz, Jennifer; Maseda, Michael; Mozena, Mark; Nandra, Kirpal; Rosario, David J.; Zeimann, Gregory R.

In: Astrophysical Journal, Vol. 793, No. 2, 101, 01.10.2014.

Research output: Contribution to journalArticle

TY - JOUR

T1 - No more active galactic nuclei in clumpy disks than in smooth galaxies at z ∼ 2 in candels/3D-HST

AU - Trump, Jonathan R.

AU - Barro, Guillermo

AU - Juneau, Stéphanie

AU - Weiner, Benjamin J.

AU - Luo, Bin

AU - Brammer, Gabriel B.

AU - Bell, Eric F.

AU - Brandt, W. N.

AU - Dekel, Avishai

AU - Guo, Yicheng

AU - Hopkins, Philip F.

AU - Koo, David C.

AU - Kocevski, Dale D.

AU - McIntosh, Daniel H.

AU - Momcheva, Ivelina

AU - Faber, S. M.

AU - Ferguson, Henry C.

AU - Grogin, Norman A.

AU - Kartaltepe, Jeyhan

AU - Koekemoer, Anton M.

AU - Lotz, Jennifer

AU - Maseda, Michael

AU - Mozena, Mark

AU - Nandra, Kirpal

AU - Rosario, David J.

AU - Zeimann, Gregory R.

PY - 2014/10/1

Y1 - 2014/10/1

N2 - We use CANDELS imaging, 3D-HST spectroscopy, and Chandra X-ray data to investigate if active galactic nuclei (AGNs) are preferentially fueled by violent disk instabilities funneling gas into galaxy centers at 1.3 < z < 2.4. We select galaxies undergoing gravitational instabilities using the number of clumps and degree of patchiness as proxies. The CANDELS visual classification system is used to identify 44 clumpy disk galaxies, along with mass-matched comparison samples of smooth and intermediate morphology galaxies. We note that despite being mass-matched and having similar star formation rates, the smoother galaxies tend to be smaller disks with more prominent bulges compared to the clumpy galaxies. The lack of smooth extended disks is probably a general feature of the z ∼ 2 galaxy population, and means we cannot directly compare with the clumpy and smooth extended disks observed at lower redshift. We find that z ∼ 2 clumpy galaxies have slightly enhanced AGN fractions selected by integrated line ratios (in the mass-excitation method), but the spatially resolved line ratios indicate this is likely due to extended phenomena rather than nuclear AGNs. Meanwhile, the X-ray data show that clumpy, smooth, and intermediate galaxies have nearly indistinguishable AGN fractions derived from both individual detections and stacked non-detections. The data demonstrate that AGN fueling modes at z ∼ 1.85 - whether violent disk instabilities or secular processes - are as efficient in smooth galaxies as they are in clumpy galaxies.

AB - We use CANDELS imaging, 3D-HST spectroscopy, and Chandra X-ray data to investigate if active galactic nuclei (AGNs) are preferentially fueled by violent disk instabilities funneling gas into galaxy centers at 1.3 < z < 2.4. We select galaxies undergoing gravitational instabilities using the number of clumps and degree of patchiness as proxies. The CANDELS visual classification system is used to identify 44 clumpy disk galaxies, along with mass-matched comparison samples of smooth and intermediate morphology galaxies. We note that despite being mass-matched and having similar star formation rates, the smoother galaxies tend to be smaller disks with more prominent bulges compared to the clumpy galaxies. The lack of smooth extended disks is probably a general feature of the z ∼ 2 galaxy population, and means we cannot directly compare with the clumpy and smooth extended disks observed at lower redshift. We find that z ∼ 2 clumpy galaxies have slightly enhanced AGN fractions selected by integrated line ratios (in the mass-excitation method), but the spatially resolved line ratios indicate this is likely due to extended phenomena rather than nuclear AGNs. Meanwhile, the X-ray data show that clumpy, smooth, and intermediate galaxies have nearly indistinguishable AGN fractions derived from both individual detections and stacked non-detections. The data demonstrate that AGN fueling modes at z ∼ 1.85 - whether violent disk instabilities or secular processes - are as efficient in smooth galaxies as they are in clumpy galaxies.

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