The H I mass function and velocity width function of void galaxies in the Arecibo Legacy Fast ALFA Survey.

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dc.careerCiencias biológicases
dc.category.authoraddeden_US
dc.contributor.authorHoyle, Fiona
dc.contributor.correspondingMoorman, Crystal M.
dc.countryEcuadores
dc.date.accessioned2023-11-04T21:36:21Z
dc.date.available2023-11-04T21:36:21Z
dc.date.issued2014
dc.dedication.authorTPes
dc.description.abstractWe measure the H i mass function (HIMF) and velocity width function (WF) across environments over a range of masses, 7.2<log(MHI/M⊙)<10.8, and profile widths, 1.3 log (km s−1) < log (W) < 2.9 log (km s−1), using a catalogue of ∼7300 H i-selected galaxies from the Arecibo Legacy Fast ALFA (ALFALFA) Survey, located in the region of sky where ALFALFA and Sloan Digital Sky Survey (Data Release 7) North overlap. We divide our galaxy sample into those that reside in large-scale voids (void galaxies) and those that live in denser regions (wall galaxies). We find the void HIMF to be well fitted by a Schechter function with normalization Φ* = (1.37 ± 0.1) × 10−2y h3 Mpc−3, characteristic mass log(M∗HI/M⊙) + 2 log h70 = 9.86 ± 0.02, and low-mass-end slope α = −1.29 ± 0.02. Similarly, for wall galaxies, we find best-fitting parameters Φ* = (1.82 ± 0.03) × 10−2 h3 Mpc−3, log(M∗HI/M⊙) + 2 log h70 = 10.00 ± 0.01, and α = −1.35 ± 0.01. We conclude that void galaxies typically have slightly lower H i masses than their non-void counterparts, which is in agreement with the dark matter (DM) halo mass function shift in voids assuming a simple relationship between DM mass and H i mass. We also find that the low-mass slope of the void HIMF is similar to that of the wall HIMF suggesting that there is either no excess of low-mass galaxies in voids or there is an abundance of intermediate H i mass galaxies. We fit a modified Schechter function to the ALFALFA void WF and determine its best-fitting parameters to be Φ* = 0.21 ± 0.1 h3 Mpc−3, log (W*) = 2.13 ± 0.3, α = 0.52 ± 0.5, and high-width slope β = 1.3 ± 0.4. For wall galaxies, the WF parameters are Φ* = 0.022 ± 0.009 h3 Mpc−3, log (W*) = 2.62 ± 0.5, α = −0.64 ± 0.2, and β = 3.58 ± 1.5. Because of large uncertainties on the void and wall WFs, we cannot conclude whether the WF is dependent on the environment.en_US
dc.facultyCiencias Exactas y Naturaleses
dc.id.author1750251827
dc.id.type1
dc.identifier.doi10.1093/mnras/stu1674
dc.identifier.issn00358711 - 13652966
dc.identifier.urihttps://repositorio.puce.edu.ec/handle/123456789/5510
dc.identifier.urihttp://mnras.oxfordjournals.org/content/444/4/3559.short
dc.indexed.databaseOtheres
dc.language.isoen
dc.list.authorsMoorman, C. M.
dc.magazine.pageRange3559-3570
dc.magazine.titleMontly Notices of the Royal Astronomical societyen_US
dc.magazine.volumeChapter444 (4)
dc.rightsClosedAccessen
dc.statepublisheden_US
dc.subjectMethodses
dc.subjectStatistical galaxieses
dc.subjectDistances and redshifts galaxieses
dc.subjectLuminosity functiones
dc.subjectMass function cosmologyes
dc.subjectObservations large-scalees
dc.subjectStructure of Universees
dc.subjectRadio lineses
dc.subjectGalaxieses
dc.subjectMethods
dc.subjectStatistical galaxies
dc.subjectDistances and redshifts galaxies
dc.subjectLuminosity function
dc.subjectMass function cosmology
dc.subjectObservations large-scale
dc.subjectStructure of Universe
dc.subjectRadio lines
dc.subjectGalaxies
dc.titleThe H I mass function and velocity width function of void galaxies in the Arecibo Legacy Fast ALFA Survey.en_US
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