J/MNRAS/501/4550 The complete Arecibo Ultra-Deep Survey (Xi+, 2021)
The Arecibo Ultra-Deep Survey.
Xi H., Staveley-smith L., For B.-Q., Freudling W., Zwaan M., Hoppmann L.,
Liang F.-H., Peng B.
<Mon. Not. R. Astron. Soc., 501, 4550-4564 (2021)>
=2021MNRAS.501.4550X 2021MNRAS.501.4550X (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, radio; H I data; Surveys
Keywords: galaxies: evolution; galaxies: ISM
galaxies: luminosity function, mass function; radio lines: galaxies
Abstract:
The Arecibo Ultra-Deep Survey (AUDS) is a blind HI survey aimed at
detecting galaxies beyond the local Universe in the 21-cm emission
line of neutral hydrogen (HI). The Arecibo L-band Feed Array (ALFA)
was used to image an area of 1.35deg2 to a redshift depth of 0.16,
using a total on-source integration time of over 700h. The long
integration time and small observation area makes it one of the most
sensitive HI surveys, with a noise level of ∼75µJy per 21.4kHz
(equivalent to 4.5km/s at redshift z=0). We detect 247 galaxies in the
survey, more than doubling the number already detected in AUDS60. The
mass range of detected galaxies is
log(MHI[h70-2M☉])=6.32-10.76. A modified maximum
likelihood method is employed to construct an H I mass function
(HIMF). The best fitting Schechter parameters are low-mass slope
α=-1.37±0.05, characteristic mass
log(M*[h70-2M☉])=10.15±0.09, and density
Φ*=(2.41±0.57)x10-3h703Mpc-3/dex. The sample was
divided into low- and high-redshift bins to investigate the evolution
of the HIMF. No change in low-mass slope α was measured, but an
increased characteristic mass M*, was noted in the higher redshift
sample. Using Sloan Digital Sky Survey data to define relative galaxy
number density, the dependence of the HIMF with environment was also
investigated in the two AUDS regions. We find no significant variation
in α or M*. In the surveyed region, we measured a cosmic HI
density ΩHI=(3.55±0.30)x10-4h70-1. There appears to be
no evolutionary trend in ΩHI above 2σ significance
between redshifts of 0 and 0.16.
Description:
We use the blind HI Arecibo Ultra-Deep Survey (AUDS) to focus on
galaxies of lower mass and at higher redshift than HIPASS or ALFALFA.
The sensitivity of AUDS is 50-200 times better than the above surveys,
but is restricted to a much smaller area and cosmic volume. AUDS also
uses the Arecibo L-band Feed Array (ALFA).
The project started in November 2008 and finished in December 2012. In
total, over 1000h observation time was assigned for the project, with
an on-source time over 700h.
The spectrometer recorded the spectral data in two sub-bands, namely
S0 and S1. The two sub-bands were centred at 1.30 and 1.45GHz,
covering a total bandwidth of 300MHz from 1.225 to 1.525GHz.
See Section 2.
In this paper, we use H0=70h70km/s/Mpc, ΩM=0.3, and
ΩΛ=0.7.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 108 247 Properties of galaxies in AUDS100 (the complete
HI Arecibo Ultra-Deep Survey)
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See also:
VIII/65 : 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998)
VIII/73 : HI Parkes All Sky Survey Catalogue (HIPASS) (Meyer+, 2004)
VIII/89 : Northern HI Parkes All Sky Survey Catalogue (HIPASS) (Wong+, 2006)
J/MNRAS/312/557 : K-band Luminosity Function of Field Galaxies (Loveday 2000)
J/MNRAS/346/1103 : Redshifts of damped Lymanα absorbers (Peroux+, 2003)
J/AJ/129/220 : HI Parkes Zone of Avoidance Survey (Donley+, 2005)
J/MNRAS/361/34 : HIPASS catalogue. III. (Doyle+, 2005)
J/ApJ/635/123 : The SDSS-DR3 damped Lyα survey (Prochaska+, 2005)
J/ApJ/636/610 : Damped Lyα systems at z<1.65 (Rao+, 2006)
J/AJ/138/338 : Arecibo Legacy Fast ALFA Survey (ALFALFA) IX. (Stierwalt+, 2009)
J/A+A/505/1087 : DLAs in SDSS-DR7 (Noterdaeme+, 2009)
J/A+A/547/L1 : SDSS-III DR9 DLA catalogue (Noterdaeme+, 2012)
J/A+A/556/A141 : ESO-UVES Advanced Data Products (EUADP) sample (Zafar+, 2013)
J/MNRAS/447/1531 : HI data collection update (Courtois+, 2015)
J/MNRAS/452/217 : HI cosmological mass density at z=5 (Crighton+, 2015)
J/ApJ/818/113 : HST observations of QSOs with medium spectra (Neeleman+, 2016)
J/AJ/151/52 : The HIZOA-S survey (Staveley-Smith+, 2016)
J/MNRAS/471/3428 : Damped Lyman Alpha systems equivalent width (Rao+, 2017)
J/MNRAS/473/1879 : VVDS14h redshift catalog (Rhee+, 2018)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- AUDS [1/247] AUDS100 identification
5- 6 I2 h RAh [8/17] Hour of right ascension (J2000) (1)
8- 9 I2 min RAm Minute of right ascension (J2000) (1)
11- 14 F4.1 s RAs Second of right ascension (J2000) (1)
15 A1 --- DE- [+] Sign of declination (J2000) (1)
16- 17 I2 deg DEd [19/22] Degree of declination (J2000) (1)
19- 20 I2 arcmin DEm Arcminute of declination (J2000) (1)
22- 23 I2 arcsec DEs Arcsecond of declination (J2000) (1)
25 A1 --- Det [b] b=Galaxies detected in both band S0 and S1
(centred at 1.30GHz and 1.45GHz)
27- 33 F7.1 km/s cz [1820.8/50005.6] Recession velocity
35- 40 F6.3 mJy.MHz Sint [0.037/49.6] Integrated flux
42- 46 F5.2 mJy Speak [0.14/40.2] Peak flux density
48- 51 F4.2 MHz W50 [0.1/2.7] Linewidth at 50% of peak
53- 57 F5.2 --- LogMHI [6.3/10.8] HI mass in logarithm in the units
of [h70-2M☉]
59- 62 F4.2 --- C [0.03/1] Completeness estimation of each galaxy
64- 66 A3 --- Set Flag for sources in "Sub" sample (2)
68 A1 --- Pro [NY] Whether source is detected by the
custom source finding algorithm
(Y=detected by program or N=detected by eye)
70- 71 I2 --- G [1/16]? Flag for confusion
73- 86 A14 --- AUDS60 Identification of AUDS60 (JHHMMSS+DDMMSS;
in Simbad;
see Hoppmann+ 2015MNRAS.452.3726H 2015MNRAS.452.3726H)
88- 89 I2 h RAOh ? Optical counterpart hour of right
ascension (J2000)
91- 92 I2 min RAOm ? Optical counterpart minute of right
ascension (J2000)
94- 97 F4.1 s RAOs ? Optical counterpart second of right
ascension (J2000)
98 A1 --- DEO- ? Optical counterpart sign of declination
(J2000)
99- 100 I2 deg DEOd ? Optical counterpart degree of declination
(J2000)
102- 103 I2 arcmin DEOm ? Optical counterpart arcminute of
declination (J2000)
105- 106 I2 arcsec DEOs ? Optical counterpart arcsecond of
declination (J2000)
108 I1 --- Opt [1/2]? Catalog of optical counterpart (3)
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Note (1): Coordinates (J2000) from the two dimensional Gaussian fit.
Note (2): We have formed a high-reliability, high-completeness sub-sample
of 148 AUDS100 galaxies ("Sub") using the following criteria:
* Frequency greater than 1.25GHz (to avoid RFI),
* Peak flux density greater than 2.5σ, where σ is the local rms
in mJy, and
* Integrated flux greater than 10.5n0.5σΔν,, where
n is number of channels over which the galaxy is detected and
Δν is channel width in MHz.
None of the negative detections satisfy the above criteria, so the
reliability for Sub should be very close to 100 per cent. In this
high-reliability sub-sample, there are 83 (56 per cent) HI sources
with spectroscopic redshifts from either SDSS or AUDSOC.
See Section 4.5.
Note (3): Optical catalog as follows:
1 = SDSS,
2 = AUDSOC: Hoppmann L. 2014, PhD thesis, Univ. Western Australia
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 22-Feb-2022