J/MNRAS/451/2303 CF-HiZELS survey (Sobral+, 2015)
CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up:
Hα, [OIII] + Hβ and [OII] luminosity functions at z=0.8, 1.4 and 2.2.
Sobral D., Matthee J., Best P.N., Smail I., Khostovan A.A.,
Milvang-Jensen B., Kim J.-W., Stott J., Calhau J., Nayyeri H., Mobasher B.
<Mon. Not. R. Astron. Soc., 451, 2303-2323 (2015)>
=2015MNRAS.451.2303S 2015MNRAS.451.2303S (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Galaxies, spectra ; Photometry ; Equivalent widths
Keywords: galaxies: evolution - galaxies: formation -
galaxies: luminosity function, mass function -
cosmology: observations - early Universe -
large-scale structure of Universe
Abstract:
We present results from the largest contiguous narrow-band survey in
the near-infrared. We have used the wide-field infrared
camera/Canada-France-Hawaii Telescope and the lowOH2 filter
(1.187±0.005µm) to survey ∼10deg2 of contiguous extragalactic
sky in the SA22 field. A total of ∼6000 candidate emission-line
galaxies are found. We use deep ugrizJK data to obtain robust
photometric redshifts. We combine our data with the High-redshift(Z)
Emission Line Survey (HiZELS), explore spectroscopic surveys (VVDS,
VIPERS) and obtain our own spectroscopic follow-up with KMOS, FMOS and
MOSFIRE to derive large samples of high-redshift emission-line
selected galaxies: 3471 Hα emitters at z=0.8, 1343 [OIII] +
Hβ emitters at z=1.4 and 572 [OII] emitters at z=2.2. We probe
comoving volumes of >106Mpc3 and find significant overdensities,
including an 8.5σ (spectroscopically confirmed) overdensity of
Hα emitters at z=0.81. We derive Hα, [OIII] + Hβ and
[OII] luminosity functions at z=0.8, 1.4, 2.2, respectively, and
present implications for future surveys such as Euclid. Our uniquely
large volumes/areas allow us to subdivide the samples in thousands of
randomized combinations of areas and provide a robust empirical
measurement of sample/cosmic variance. We show that surveys for
star-forming/emission-line galaxies at a depth similar to ours can
only overcome cosmic-variance (errors <10 percent) if they are based
on volumes >5x105Mpc3; errors on L* and φ* due to sample
(cosmic) variance on surveys probing ∼104 and ∼105Mpc3 are
typically very high: ∼300 and ∼40-60 percent, respectively.
Description:
Observations were made with the CFHT using the WIRCam during three
semesters in queued service mode (Program IDs 2011B/029, 2012A019 and
2012B/016). Data were obtained using the LowOH2 NB filter (central
wavelength of 1187nm2 and a full width at half-maximum,
Δλ=10nm, also referred in this paper as NBJ), and cover
a contiguous region of ∼10deg2 (∼3x3deg2) in the SA22 field
(centred at 22:16:00, +00:18:00).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 104 6315 The catalogue of all Sigma>3 NB sources selected
in the SA22 field from this paper
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- --- [CFHIZELS-SM14-]
15- 20 A6 --- CFHIZELS CFHIZELS identification number
22- 30 F9.5 deg RAdeg Narrow band right ascension (J2000)
32- 40 F9.5 deg DEdeg Narrow band declination (J2000)
42- 48 F7.4 mag NBJmag NBJ magnitude in 2" aperture (AB)
50- 56 F7.4 mag e_NBJmag rms uncertainty on NBJmag
58- 64 F7.4 mag Jmag UKIDSS J magnitude in 2" aperture (AB)
66- 72 F7.4 mag e_Jmag rms uncertainty on Jmag
74- 79 F6.1 --- Sigma Sigma parameter
(Bunker et al., 1995MNRAS.273..513B 1995MNRAS.273..513B) (1)
81- 88 F8.4 [mW/m2] logFlux Flux of emission lines
90-100 F11.4 0.1nm EW Equivalent width of emission lines
103-104 A2 --- Class Classification flag (2)
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Note (1): The parameter Sigma is used to quantify the real excess compared to
an excess due to random scatter.
Note (2): Classification flag as follows:
-1 = potential star
0 = other lines/unclassified line emitter
1 = Hα emitter
2 = [OIII]+Hβ line emitter
3 = [OII] line emitter
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 13-Jan-2016