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

W.J.G. de Blok, K.M. Keating, D.J. Pisano, F. Fraternali, F. Walter, T. Oosterloo, E. Brinks, F. Bigiel, A. Leroy

Research output: Contribution to journalArticlepeer-review

17 Citations (Scopus)
213 Downloads (Pure)


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
Original languageEnglish
Article numberA68
Number of pages11
JournalAstronomy & Astrophysics
Publication statusPublished - 25 Sept 2014


  • galaxies: ISM, galaxies: kinematics and dynamics, galaxies: halos, galaxies: individual: NGC 2403, galaxies: structure


Dive into the research topics of 'A low H I column density filament in NGC 2403: signature of interaction or accretion'. Together they form a unique fingerprint.

Cite this