4.6 Article

Investigating the link between inner gravitational potential and star-formation quenching in CALIFA galaxies

期刊

ASTRONOMY & ASTROPHYSICS
卷 665, 期 -, 页码 -

出版社

EDP SCIENCES S A
DOI: 10.1051/0004-6361/202243541

关键词

galaxies: evolution; galaxies: kinematics and dynamics; galaxies: star formation; galaxies: fundamental parameters; galaxies: structure; galaxies: bulges

资金

  1. Deutsche Forschungsgemeinschaft, DFG [SFB956A]
  2. Conacyt [CB-285080, FC-2016-01 1916, PAPIIT-DGAPA IN100519]
  3. State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa [SEV-2017-0709]
  4. Natural Sciences and Engineering Research Council of Canada (NSERC) [RGPIN-2017-03987]
  5. [AYA2016-77846-P]
  6. [PID2019109067-GB100]

向作者/读者索取更多资源

It has been suggested that gravitational potential can play a significant role in suppressing star formation in nearby galaxies. To investigate this scenario, we studied the connection between dynamics and star formation quenching in 215 non-active galaxies. Our results show that galaxies with similar gravitational potential tend to exhibit a certain pattern of star formation quenching. Further analysis reveals that both the amplitude and shape of the gravitational potential are important factors in the quenching history of a galaxy.
It has been suggested that gravitational potential can have a significant role in suppressing star formation in nearby galaxies. To establish observational constraints on this scenario, we investigated the connection between the dynamics - taking the circular velocity curves (CVCs) as a proxy for the inner gravitational potential - and star formation quenching in 215 non-active galaxies across the Hubble sequence from the Calar Alto Legacy Integral Field Area (CALIFA) survey. Our results show that galaxies with similar CVCs tend to have a certain star-formation quenching pattern. To explore these findings in more details, we constructed kiloparsec (kpc) resolved relations of the equivalent width of the H alpha (W-H alpha) versus the amplitude (V-c) and shape (beta = dln V-c/d ln R) of the circular velocity at given radii. We find that the W-H alpha V-c is a declining relationship, where the retired regions of the galaxies (the ones with W-H alpha values of below 3 angstrom) tend to have higher V-c. Concurrently, W-H alpha-beta is a bimodal relationship, which is characterised by two peaks: concentration of the star forming regions at a positive beta (rising CVC) and a second concentration of the retired regions with a negative beta (declining CVC). Our results show that both the amplitude of the CVC - driven by the mass of the galaxies - and its shape - which reflects the internal structure of the galaxies - play an important role in the quenching history of a galaxy.

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