A low H I column density filament in NGC 2403: signature of interaction or accretion

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dc.contributor.authorde Blok, W J G
dc.contributor.authorKeating, K M
dc.contributor.authorPisano, D J
dc.contributor.authorFraternali, F
dc.contributor.authorWalter, F
dc.contributor.authorOosterloo, T
dc.contributor.authorBrinks, E
dc.contributor.authorBigiel, F
dc.contributor.authorLeroy, A
dc.date.accessioned2021-10-08T11:01:11Z
dc.date.available2021-10-08T11:01:11Z
dc.date.issued2014
dc.description.abstractObserved H i accretion around nearby galaxies can only account for a fraction of the gas supply needed to sustain the currently observed star formation rates. It is possible that additional accretion occurs in the form of low column density cold flows, as predicted by numerical simulations of galaxy formation. To constrain the presence and properties of such flows, we present deep H i observations obtained with the NRAO Green Bank Telescope of an area measuring 4° × 4° around NGC 2403. These observations, with a 5σ detection limit of 2.4 × 1018 cm-2 over a 20 km s-1 linewidth, reveal a low column density, extended cloud outside the main H i disk, about 17′ (~ 16 kpc or ~ 2 R25) to the NW of the center of the galaxy. The total H i mass of the cloud is 6.3 × 106 M⊙, or 0.15 percent of the total H i mass of NGC 2403. The cloud is associated with an 8 kpc anomalous-velocity H i filament in the inner disk, that was previously observed in deep VLA observations. We discuss several scenarios for the origin of the cloud, and conclude that it is either accreting from the intergalactic medium, or is the result of a minor interaction with a neigboring dwarf galaxy
dc.identifier.apacitationde Blok, W. J. G., Keating, K. M., Pisano, D. J., Fraternali, F., Walter, F., Oosterloo, T., ... Leroy, A. (2014). A low H I column density filament in NGC 2403: signature of interaction or accretion. <i>Astronomy and Astrophysics</i>, 569(4), A68 - 177. http://hdl.handle.net/11427/35102en_ZA
dc.identifier.chicagocitationde Blok, W J G, K M Keating, D J Pisano, F Fraternali, F Walter, T Oosterloo, E Brinks, F Bigiel, and A Leroy "A low H I column density filament in NGC 2403: signature of interaction or accretion." <i>Astronomy and Astrophysics</i> 569, 4. (2014): A68 - 177. http://hdl.handle.net/11427/35102en_ZA
dc.identifier.citationde Blok, W.J.G., Keating, K.M., Pisano, D.J., Fraternali, F., Walter, F., Oosterloo, T., Brinks, E. & Bigiel, F. et al. 2014. A low H I column density filament in NGC 2403: signature of interaction or accretion. <i>Astronomy and Astrophysics.</i> 569(4):A68 - 177. http://hdl.handle.net/11427/35102en_ZA
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.ris TY - Journal Article AU - de Blok, W J G AU - Keating, K M AU - Pisano, D J AU - Fraternali, F AU - Walter, F AU - Oosterloo, T AU - Brinks, E AU - Bigiel, F AU - Leroy, A AB - Observed H i accretion around nearby galaxies can only account for a fraction of the gas supply needed to sustain the currently observed star formation rates. It is possible that additional accretion occurs in the form of low column density cold flows, as predicted by numerical simulations of galaxy formation. To constrain the presence and properties of such flows, we present deep H i observations obtained with the NRAO Green Bank Telescope of an area measuring 4° × 4° around NGC 2403. These observations, with a 5σ detection limit of 2.4 × 1018 cm-2 over a 20 km s-1 linewidth, reveal a low column density, extended cloud outside the main H i disk, about 17′ (~ 16 kpc or ~ 2 R25) to the NW of the center of the galaxy. The total H i mass of the cloud is 6.3 × 106 M⊙, or 0.15 percent of the total H i mass of NGC 2403. The cloud is associated with an 8 kpc anomalous-velocity H i filament in the inner disk, that was previously observed in deep VLA observations. We discuss several scenarios for the origin of the cloud, and conclude that it is either accreting from the intergalactic medium, or is the result of a minor interaction with a neigboring dwarf galaxy DA - 2014 DB - OpenUCT DP - University of Cape Town IS - 4 J1 - Astronomy and Astrophysics LK - https://open.uct.ac.za PY - 2014 SM - 0004-6361 SM - 1432-0746 T1 - A low H I column density filament in NGC 2403: signature of interaction or accretion TI - A low H I column density filament in NGC 2403: signature of interaction or accretion UR - http://hdl.handle.net/11427/35102 ER - en_ZA
dc.identifier.urihttp://hdl.handle.net/11427/35102
dc.identifier.vancouvercitationde Blok WJG, Keating KM, Pisano DJ, Fraternali F, Walter F, Oosterloo T, et al. A low H I column density filament in NGC 2403: signature of interaction or accretion. Astronomy and Astrophysics. 2014;569(4):A68 - 177. http://hdl.handle.net/11427/35102.en_ZA
dc.language.isoeng
dc.publisher.departmentDepartment of Astronomy
dc.publisher.facultyFaculty of Science
dc.sourceAstronomy and Astrophysics
dc.source.journalissue4
dc.source.journalvolume569
dc.source.paginationA68 - 177
dc.source.urihttps://dx.doi.org/10.1051/0004-6361/201423880
dc.subject.othergalaxies: ISM, galaxies: kinematics and dynamics, galaxies: halos, galaxies: individual: NGC 2403, galaxies: structure
dc.subject.othergalaxies: ISM
dc.subject.othergalaxies: kinematics and dynamics
dc.subject.othergalaxies: halos
dc.subject.othergalaxies: individual: NGC 2403
dc.subject.othergalaxies: structure
dc.subject.otherArticle
dc.titleA low H I column density filament in NGC 2403: signature of interaction or accretion
dc.typeJournal Article
uct.type.publicationResearch
uct.type.resourceJournal Article
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