Skip navigation
  • INAF logo
  • Home
  • Communities
    & Collections
  • Research outputs
  • Researchers
  • Organization units
  • Projects
  • Explore by
    • Research outputs
    • Researchers
    • Organization units
    • Projects
  • Login:
    • My DSpace
    • Receive email
      updates
    • Edit Account details
  • Italian
  • English

  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/29556
Title: GASP XIII. Star formation in gas outside galaxies
Authors: POGGIANTI, Bianca Maria 
GULLIEUSZIK, MARCO 
Tonnesen, Stephanie
MORETTI, ALESSIA 
Vulcani, Benedetta 
RADOVICH, MARIO 
Jaffé, Yara
Fritz, Jacopo
BETTONI, Daniela 
FRANCHETTO, ANDREA
FASANO, Giovanni
BELLHOUSE, CALLUM 
Omizzolo, Alessandro
Issue Date: 2019
Journal: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 
Number: 482
Issue: 4
First Page: 4466
Abstract: Based on MUSE data from the GASP survey, we study the H α-emitting extraplanar tails of 16 cluster galaxies at z ∼ 0.05 undergoing ram pressure stripping. We demonstrate that the dominating ionization mechanism of this gas (between 64 per cent and 94 per cent of the H α emission in the tails depending on the diagnostic diagram used) is photoionization by young massive stars due to ongoing star formation (SF) taking place in the stripped tails. This SF occurs in dynamically quite cold H II clumps with a median H α velocity dispersion σ = 27 km s^{-1}. We study the characteristics of over 500 star-forming clumps in the tails and find median values of H α luminosity L_{H α } = 4× 10^{38} erg s^{-1}, dust extinction A<SUB>V</SUB> = 0.5 mag, star formation rate SFR=0.003 M_{☉} yr^{-1}, ionized gas density n_e =52 cm^{-3}, ionized gas mass M_gas = 4× 10^4 M_{☉}, and stellar mass M_{*} = 3× 10^6 M_{☉}. The tail clumps follow scaling relations (M<SUB>gas</SUB> - M<SUB>*</SUB>, L<SUB>H α</SUB> - σ, SFR-M<SUB>gas</SUB>) similar to disc clumps, and their stellar masses are comparable to Ultra Compact Dwarfs and Globular Clusters. The diffuse gas component in the tails is ionized by a combination of SF and composite/LINER-like emission likely due to thermal conduction or turbulence. The stellar photoionization component of the diffuse gas can be due either to leakage of ionizing photons from the H II clumps with an average escape fraction of 18 per cent, or lower luminosity H II regions that we cannot individually identify.
URI: http://hdl.handle.net/20.500.12386/29556
URL: https://academic.oup.com/mnras/article-abstract/482/4/4466/5161243
ISSN: 0035-8711
DOI: 10.1093/mnras/sty2999
Bibcode ADS: 2019MNRAS.482.4466P
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

Files in This Item:
File Description SizeFormat 
1811.00823.pdf23.72 MBAdobe PDFView/Open
sty2999.pdfPDF editoriale32.51 MBAdobe PDFView/Open
Show full item record

Page view(s)

6
checked on Jan 25, 2021

Download(s)

1
checked on Jan 25, 2021

Google ScholarTM

Check

Altmetric


Items in DSpace are published in Open Access, unless otherwise indicated.


Explore by
  • Communities
    & Collections
  • Research outputs
  • Researchers
  • Organization units
  • Projects

Informazioni e guide per autori

https://openaccess-info.inaf.it: tutte le informazioni sull'accesso aperto in INAF

Come si inserisce un prodotto: le guide a OA@INAF

La Policy INAF sull'accesso aperto

Documenti e modelli scaricabili

Feedback
Built with DSpace-CRIS - Extension maintained and optimized by Logo 4SCIENCE