NIBLES – an HI census of stellar mass selected SDSS galaxies

Butcher, Z.; Schneider, Stephen E.; Driel, W. van; Lehnert, M. D.; Minchin, R. F.

doi:10.1051/0004-6361/201628189

Cited by 7 publications

(7 citation statements)

References 39 publications

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“…at Arecibo for a fraction of the galaxies that were either not detected or marginally detected; 80% of them were detected with HI masses ∼ 0.5 dex lower than the upper limits in , and the rest, mostly luminous red galaxies, were not detected. If this trend is representative of the rest of the NRT undetected galaxies, Butcher et al (2016) expect the fit plotted in Fig. 15 to be offset toward lower R HI values by about 0.17 dex and even more at the highest masses.…”

Section: Comparisons With Previous Workmentioning

confidence: 90%

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The $HI$- and $H_{2}$-to-stellar mass correlations of late- and early-type galaxies and their consistency with the observational mass functions

Calette¹,

Ávila-Reese²,

Rodríguez-Puebla³

et al. 2018

Preprint

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muestras locales de galaxias que contienen información de la masa estelar, de HI y/o H 2 , y morfología. Procesamos adecuadamente la información relacionada con las no detecciones en gas y determinamos la relaciones de masa estelar a masa de HI y H 2 y sus dispersiones, tanto para galaxias tardías como tempranas. Las relaciones se describen por leyes simples o doble de potencias; las respectivos cocientes de masa H 2 a HI son presentados. Contreñimos también las distribuciones completas de los cocientes de masa de HI y H 2 a masa estelar, encontrando que se describen bien por una función de Schechter (galaxias tardías) y una función Schechter (cortada) + uniforme (galaxias tempranas). Usando la función de masa estelar y el cociente de galaxias tempranas a tardías en función de M * , estas distribuciones son mapeadas en funciones de masa de HI y H 2 . Las funciones de masa obtenidas son consistentes con aquellas inferidas de catastros. Las relaciones empíricas de masa de gas a estrellas y sus distribuciones para galaxias tardías/tempranas presentadas aquí pueden ser usadas para constreñir modelos y simulaciones de evolución de galaxias.

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Section: Comparisons With Previous Workmentioning

confidence: 90%

“…Their fit is for all the sample, that is, they do not separate into LTG/ETG or blue/red groups. In a subsequent paper (Butcher et al 2016), the authors obtained ∼ 4 times more sensitive follow-up HI observations Fig. 15.…”

Section: Comparisons With Previous Workmentioning

confidence: 94%

The $HI$- and $H_{2}$-to-stellar mass correlations of late- and early-type galaxies and their consistency with the observational mass functions

Calette¹,

Ávila-Reese²,

Rodríguez-Puebla³

et al. 2018

Preprint

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“…This "derippling" was performed by M.D. Lehnert, using a Python routine written by him (see Butcher et al 2016) In our adjudication of detections, we divided them into four categories: clear, marginal, possible and non-detections. This is based on independent visual inspections of the spectra as well as on the S/N parameter (cf.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

The Nançay H i Zone of Avoidance survey of 2MASS bright galaxies

Kraan-Korteweg

Driel

Schröder

et al. 2018

Monthly Notices of the Royal Astronomical Society

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To complement the 2MASS Redshift Survey (2MRS) and the 2MASS Tully-Fisher survey (2MTF) a search for 21cm H I line emission of 2MASS bright galaxy candidates has been pursued along the dust-obscured plane of the Milky Way with the 100m Nançay Radio Telescope. For our sample selection we adopted an isophotal extinction-corrected K s -band magnitude limit of K o s = 11. m 25, corresponding to the first 2MRS data release and 2MTF, for which the 2MASX completeness level remains fairly constant deep into the Zone of Avoidance (ZoA). About one thousand galaxies without prior redshift measurement accessible from Nançay (Dec > −40 • ) were observed to an rms noise level of ∼ 3 mJy for the velocity range −250 to 10 600 km s −1 . This resulted in 220 clear and 12 marginal detections of the target sample. Only few detections have redshifts above 8000 km s −1 due to recurring radio frequency interference (RFI). A further 29 detections and 6 marginals have their origin in nontarget galaxies in the telescope beam. The newly detected galaxies are on average considerably more H I-rich (mostly 10 9 − 10 10 M ⊙ ) compared to systematic (blind) H I surveys. The H I detections reveal various new filaments crossing the mostly uncharted northern ZoA (e.g. at ℓ ∼ 90 • , 130 • , 160 • ), whilst consolidating galaxy agglomerations in Monoceros and Puppis (ℓ ∼ 220 • , 240 • ). Considerably new insight has been gained about the extent of the Perseus-Pisces Supercluster through the confirmation of a ridge (ℓ ∼ 160 • ) encompassing the 3C129 cluster that links Perseus-Pisces to Lynx, and the continuation of the second Perseus-Pisces arm (ℓ ∼ 90 • ) across the ZoA.

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“…However, there is a currently unknown Hi distribution lying below the detection threshold of NIBLES which will expand the plane of the BLF if probed. We are currently working on implementing a BLF incorporating four times more sensitive follow-up observations of the NIBLES undetected sample with the Arecibo L-band wideband receiver (see also the pilot survey results in Butcher et al 2016).…”

Section: Future Workmentioning

confidence: 99%

Bivariate luminosity-HI mass distribution function of galaxies based on the NIBLES survey

Butcher

Schneider

Driel

et al. 2018

A&A

Self Cite

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We present a new optical luminosity-Hi mass bivariate luminosity function (BLF) based on Hi line observations from the Nançay Interstellar Baryons Legacy Extragalactic Survey (NIBLES). NIBLES sources lie within the local universe (900 ≤ cz ≤ 12,000 km s −1 ) and were chosen from SDSS DR5 such that the optical luminosity function was sampled as uniformly as possible. The Hi mass function (HIMF) derived from our raw-data BLF, which is based on Hi detections only, is consistent with the HIMFs derived from other optically selected surveys in that the low-mass slope is flatter than those derived from blind Hi surveys. However, spanning the entire luminosity range of NIBLES, we identify a highly consistent distribution of the Hi gas mass to luminosity ratio (gas-to-light ratio) with a predictable progression in the mean M HI /L r ratio as a function of L r . This consistency allows us to construct plausible gasto-light ratio distributions for very low-luminosity bins which lie outside the NIBLES sample. We also identify a ∼ 10% decrease in detection fraction for galaxies fainter than log(L r ) = 9.25, consistent with the expected decrease due to distance and sensitivity effects. Accounting for these trends, we reconstruct plausible gas-to-light distributions spanning luminosity bins down to log(L r ) = 5.25, thus producing a corrected BLF. This corrected BLF is in good qualitative agreement with optical luminosity-Hi mass distributions from the ALFALFA survey and is able to accurately reproduce blind survey HIMFs, lending credibility that this two dimensional optical luminosity-Hi mass distribution is an accurate representation of the volume density distribution of galaxies in the local universe. We also note that our agreement with HIMFs from other surveys is dependent on accounting for all systematic differences such as selection method, Hubble constant and Hi flux scale.

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NIBLES – an HI census of stellar mass selected SDSS galaxies

Cited by 7 publications

References 39 publications

The $HI$- and $H_{2}$-to-stellar mass correlations of late- and early-type galaxies and their consistency with the observational mass functions

The $HI$- and $H_{2}$-to-stellar mass correlations of late- and early-type galaxies and their consistency with the observational mass functions

The Nançay H i Zone of Avoidance survey of 2MASS bright galaxies

Bivariate luminosity-HI mass distribution function of galaxies based on the NIBLES survey

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