1. RRI Digital Repository
  2. 04. Astronomy and Astrophysics
  3. Research Papers (A&A)
Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7786
Full metadata record
DC FieldValueLanguage
dc.contributor.authorYadav, Jyoti-
dc.contributor.authorDas, Mousumi-
dc.contributor.authorPatra, Narendra Nath-
dc.contributor.authorDwarakanath, K. S.-
dc.contributor.authorRahna, P. T.-
dc.contributor.authorMcGaugh, Stacy S.-
dc.contributor.authorJames Schombert, Stacy S.-
dc.contributor.authorMurthy, Jayant-
dc.date.accessioned2021-06-29T06:38:54Z-
dc.date.available2021-06-29T06:38:54Z-
dc.date.issued2021-06-
dc.identifier.citationThe Astrophysical Journal, 2021, Vol.914, p54en_US
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357(Online)-
dc.identifier.urihttp://hdl.handle.net/2289/7786-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractWe present a far-UV (FUV) study of the star-forming complexes (SFCs) in three nearby galaxies using the Ultraviolet Imaging Telescope. The galaxies are close to face-on and show significant outer disk star formation. Two of them are isolated (NGC 628 and NGC 6946), and one is interacting with distant companions (NGC 5457). We compared the properties of the SFCs inside and outside the optical radius (R25). We estimated the sizes, star formation rates (SFRs), metallicities, and Toomre Q parameter of the SFCs. We find that the outer disk SFCs are at least 10 times smaller in area than those in the inner disk. The SFRs per unit area (ΣSFR) in both regions have similar mean values, but the outer SFCs have a much smaller range of ΣSFR. They are also metal-poor compared to the inner disk SFCs. The FUV emission is well correlated with the neutral hydrogen gas (H i) distribution and detected within and near several H i holes. Our estimation of the Q parameter in the outer disks of the two isolated galaxies suggests that their outer disks are stable (Q > 1). However, their FUV images indicate that there is ongoing star formation in these regions. This suggests that there may be some nonluminous mass or dark matter in their outer disks, which increases the disk surface density and supports the formation of local gravitational instabilities. In the interacting galaxy, NGC 5457, the baryonic surface density is sufficient (Q < 1) to trigger local disk instabilities in the outer disk.en_US
dc.language.isoenen_US
dc.publisherIOP Sciences for The American Astronomical Societyen_US
dc.relation.urihttps://arxiv.org/abs/2103.16819en_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/abf8c1en_US
dc.rights2021, The American Astronomical Societyen_US
dc.subjectUltraviolet astronomy (1736)en_US
dc.subjectSpiral galaxies (1560)en_US
dc.subjectGalaxy interactions (600)en_US
dc.subjectStar forming regions (1565)en_US
dc.subjectHI shells (728)en_US
dc.titleComparing the Inner and Outer Star-forming Complexes in the Nearby Spiral Galaxies NGC 628, NGC 5457, and NGC 6946 Using UVIT Observationsen_US
dc.typeArticleen_US
Appears in Collections:Research Papers (A&A)

Files in This Item:
File Description SizeFormat 
2021_ApJ_914_54.pdf
  Restricted Access		Restricted Access2.64 MBAdobe PDFView/Open Request a copy
Show simple item record


Items in RRI Digital Repository are protected by copyright, with all rights reserved, unless otherwise indicated.