Λcdm Satellites and H I Companions—the Arecibo Alfa Survey of NGC 2903

Irwin, Judith A.; Hoffman, G. L.; Spekkens, Kristine; Haynes, Martha P.; Giovanelli, Riccardo; Linder, Suzanne M.; Catinella, Barbara; Momjian, Emmanuel; Koribalski, B. S.; Davies, Jonathan Ivor; Brinks, E.; Blok, W. J. G. de; Putman, Mary E.; Driel, W. van

doi:10.1088/0004-637x/692/2/1447

Cited by 45 publications

(49 citation statements)

References 94 publications

(130 reference statements)

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“…A total of ∼30 000 galaxies are expected to be detected. The first galaxy catalogs are Giovanelli et al (2007), Saintonge et al (2008), Kent et al (2008), Martin et al (2009), Stierwalt et al (2009), the subsequent α.40 catalog (Haynes et al 2011) Cortese et al (2008), Irwin et al (2009), Minchin et al (2010, Davies et al (2011), Taylor et al (2012, 2014a, Minchin et al (2016), Keenan et al (2016); 4. GASS: pointed survey at the Arecibo 305 m telescope (Catinella et al 2012) of 666 galaxies with stellar masses greater than 10 10 M selected from the SDSS spectroscopic and the Galaxy Evolution Explorer (GALEX) ultraviolet imaging surveys.…”

Section: Introductionmentioning

confidence: 99%

NIBLES: an H I census of stellar mass selected SDSS galaxies

Driel

Butcher

Schneider

et al. 2016

A&A

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To investigate galaxy properties as a function of their total stellar mass, we obtained 21 cm H i line observations at the 100-m class Nançay Radio Telescope of 2839 galaxies from the Sloan Digital Sky Survey (SDSS) in the Local Volume (900 < cz < 12 000 km s −1 ), dubbed the Nançay Interstellar Baryons Legacy Extragalactic Survey (NIBLES) sample. They were selected evenly over their entire range of absolute SDSS z-band magnitudes (M z ∼ −13.5 to −24 mag), which were used as a proxy for their stellar masses. In this paper, a first, global presentation of the observations and basic results is given; their further analysis will be presented in other papers in this series. The galaxies were originally selected based on their properties, as listed in SDSS DR5. Comparing this photometry to their total H i masses, we noted that, for a few percent, the SDSS magnitudes appeared severely misunderestimated, as confirmed by our re-measurements for selected objects. Although using the later DR9 results eliminated this problem in most cases, 384 still required manual photometric source selection. Usable H i spectra were obtained for 2600 of the galaxies, of which 1733 (67%) were clearly detected and 174 (7%) marginally. The spectra for 241 other observed galaxies could not be used for further analysis owing to problems with either the H i or the SDSS data. We reached the target number of about 150 sources per half-magnitude bin over the M z range −16.5 to −23 mag. Down to −21 mag the overall detection rate is rather constant at the ∼75% level but it starts to decline steadily towards the 30% level at −23 mag. Making regression fits by comparing total H i and stellar masses for our sample, including our conservatively estimated H i upper limits for non-detections, we find the relationship log(M H I /M ) = −0.59 log(M ) + 5.05, which lies significantly below the relationship found in the M H I /M -M plane when only using H i detections.

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Section: Introductionmentioning

confidence: 99%

NIBLES: an H I census of stellar mass selected SDSS galaxies

Driel

Butcher

Schneider

et al. 2016

A&A

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“…Recent work (Irwin et al 2009) on the H i content of NGC 2903 has shown that it possesses a large H i envelope of around three times its optical size. They also found a small H i companion 64 kpc away from the galaxy in projection, which adds to a previously known small stellar companion.…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength study of the star-formation in the bar of NGC 2903

Popping¹,

Pérez

Zurita

2010

A&A

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Aims. NGC 2903 is a nearby barred spiral with an active starburst in the center and H ii regions distributed along its bar. We aim to analyse the star formation properties in the bar region of NGC 2903 and study the links with the typical bar morphological features. Methods. A combination of space and ground-based data from the far-ultraviolet to the sub-millimeter spectral ranges is used to create a panchromatic view of the NGC 2903 bar. We produce two catalogues: one for the current star formation regions, as traced by the Hα compact emission, and a second one for the ultraviolet (UV) emitting knots, containing positions and luminosities. From them we have obtained ultraviolet colours, star formation rates, dust attenuation and Hα EWs, and their spatial distribution have been analysed. Stellar cluster ages have been estimated using stellar population synthesis models (Starburst99). Results. NGC 2903 is a complex galaxy, with a very different morphology on each spectral band. The CO (J=1-0) and the 3.6 µm emission trace each other in a clear barred structure, while the Hα leads both components and it has an s-shape distribution. The UV emission is patchy and does not resemble a bar. The UV emission is also characterised by a number of regions located symmetrically with respect to the galaxy center, almost perpendicular to the bar, in a spiral shape covering the inner ∼ 2.5kpc. These regions do not show a significant Hα nor 24 µm emission. We have estimated ages for these regions ranging from 150 to 320 Myr, being older than the rest of the UV knots, which have ages lower than 10 Myr. The SFR calculated from the UV emission is ∼0.4 M ⊙ yr −1 , compatible with the SFR as derived from Hα calibrations (∼1 M ⊙ yr −1 ).

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“…These anomalous H I clouds appear to be the analogs of the large HVC complexes in the MW with substantial H I masses, large extents of several kpcs and projected separations from the galactic disks of ∼ 10 − 20 kpc. Other dedicated surveys of other nearby galaxies and galaxy groups reveal no HVC analogs down to ∼ 4 × 10 5 M at larger distances from galaxies (Pisano et al 2007;Irwin et al 2009). …”

Section: Pos(aaska14)129mentioning

confidence: 87%

The SKA view of the Neutral Interstellar Medium in Galaxies

Blok¹,

Fraternali²,

Heald³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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Two major questions in galaxy evolution are how star-formation on small scales leads to global scaling laws and how galaxies acquire sufficient gas to sustain their star formation rates. H I observations with high angular resolution and with sensitivity to very low column densities are some of the important observational ingredients that are currently still missing. Answers to these questions are necessary for a correct interpretation of observations of galaxy evolution in the high-redshift universe and will provide crucial input for the sub-grid physics in hydrodynamical simulations of galaxy evolutions. In this chapter we discuss the progress that will be made with the SKA using targeted observations of nearby individual disk and dwarf galaxies.Advancing Astrophysics with the Square Kilometre Array

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Λcdm Satellites and H I Companions—the Arecibo Alfa Survey of NGC 2903

Cited by 45 publications

References 94 publications

NIBLES: an H I census of stellar mass selected SDSS galaxies

NIBLES: an H I census of stellar mass selected SDSS galaxies

Multiwavelength study of the star-formation in the bar of NGC 2903

The SKA view of the Neutral Interstellar Medium in Galaxies

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