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Review meeting for ALMA deep survey
2013-010-24
MAHALO sample in CANDELS-SXDF field
Tadaki, K., Kodama, T., Tanaka, I., Koyama, Y. (NAOJ),
Hayashi, M. (Univ. of Tokyo), Shimakawa, R. (GUAS)
1. Band-3 survey in cycle-1 ALMA field (Kohno et al.)
2. Band-6 high-resolution (<0.2″) observations pointing Hα-selected galaxies at
z=1.5-2.5
3. Band-6 low-resolution (0.5″) deep survey in cycle-1 ALMA field
2
Tadaki et al.
MAHALO-Subaru project (PI: T. Kodama)
1.0
2.1
2.2
Redshift
2.3 2.4 2.5
NB209
2.6
2.7
TABLE 1
Multi-wavelength data.
2.8
NB2315
K
0.8
Filter
u
B
V
Rc
i!
z!
Y
Ks
J
H
K
3.6µm
4.5µm
Transmission
SXDF-UDS-CADELS field
0.6
0.4
0.2
0.0
2.0
2.1
2.2
2.3
2.4
2.5
Wavelength [µm]
Fig. 1.— The transmission curves of NB209 and NB2315 filters
on MOIRCS (solid line) and the WFCAM K-band filter (dashed
line). The labels on the top axis indicate redshifts for Hα emitters.
cycle-1 ALMA field (Kohno et al)
Instrument
CFHT/MegaCam
Subaru/Suprime-Cam
Subaru/Suprime-Cam
Subaru/Suprime-Cam
Subaru/Suprime-Cam
Subaru/Suprime-Cam
VLT/HAWK-I
VLT/HAWK-I
UKIRT/WFCAM
UKIRT/WFCAM
UKIRT/WFCAM
Spitzer/IRAC
Spitzer/IRAC
m5σ,AB
27.68
28.38
28.01
27.78
27.69
26.67
26.69
25.92
25.63
24.76
25.39
24.72
24.61
Reference
Almaini et a
Furusawa et al.
Furusawa et al.
Furusawa et al.
Furusawa et al.
Furusawa et al.
Fontana et a
Fontana et a
Lawrence et al.
Lawrence et al.
Lawrence et al.
Ashby et al
Ashby et al
Transmission
1.0Subaru/XM M –N ewton Deep survey Field (SXDF;
sequence galaxies represent 98% of mass-selected starrusawa etNB209
al. 2008). We show the target selection
forming galaxies and account for ∼90% of the cosmic
Hα emitters in Section 3. In Section
4, their global p
K
SFR density at z ∼ 2, with the sample detected by
0.8
erties such as SFRs, stellar masses and metallicities
PACS 100 µm or 160 µm on-board Herschel as well as
derived, andHα輝線
the mass-metallicity relation is presen
optical/near-infrared (NIR) color-selected one. Despite
0.6In Section 5, we discuss the main-sequence galaxie
its importance, the definition of main sequence is largely
(z=2.2)
z > 2 and the dustiness of star formation activities.
dependent on a sample selection and a SFR indicator
summarize our study in Section 6. Throughout this
used. In this paper, we present the main sequence of
0.4per, we assume the cosmological parameters of H
0
star-forming galaxies at z > 2, which are selected from
−1
−1
km s Mpc , ΩM = 0.3, and ΩΛ = 0.7, and Salp
a Hα narrow-band (NB) imaging survey. The advantage
of selecting galaxies with a NB imaging is that we can
0.2IMF is adopted for the estimation of stellar masses
SFRs (Salpeter 1955).
construct a nearly SFR-limited, complete sample of starforming galaxies ~15′
which spans a broader range in stellar
2. DATA
0.0
massinfrom
Mstar ∼ 109 M! (e.g. Lyman break galaxies;
Tadaki+13a,
press
2.0
2.1
2.2
2.3
2.4
2.5
11
We
have
conducted
the
Hα
emitter
surveys in
LBGs) to Mstar > 10 M! (e.g. submillimeter-selected
Wavelength [µm]
redshift slices at z = 2.2 and at z = 2.5 in par
galaxies; SMGs). Also, a Hα line is one of the best SFR
major general
field SXDF.
Two narrow-band
indicators
as well asproject
a probe oftargets
high-z star-forming
MAHALO
the peakgalaxepoch the
of galaxy
formation
(z~2).
ters, namely NB209 (λc = 2.09µm, FWHM=0.027
ies, which has many great advantages: being less affected
and NB2315 (λ = 2.315µm, FWHM=0.027µm)
MAHALO-Subaru project (PI: T. Kodama)
SXDF-UDS-CADELS field
Dec. [arcmin]
cycle-1 ALMA field (Kohno et al)
0
24µm
NB209-6
V606
I814
J125
H160
M
24µm
NB209-7
V606
I814
J125
H160
M
24µm
NB209-12
V606
I814
J125
H160
M
24µm
NB2315-1
V606
I814
J125
H160
M
24µm
NB2315-4
V606
I814
J125
H160
M
z=2.2 HAE
5
0
-5
Dec. [arcmin]
R.A. [arcmin]
0
z=2.5 HAE
5
0
R.A. [arcmin]
-5
Tadaki+13b, submitted
MAHALO-Subaru project (PI: T. Kodama)
SXDF-UDS-CADELS field
Dec. [arcmin]
VLT/KMOS field (Koyama et al)
22 HAEs will be observed by KMOS.
0
Five KMOS targets (z=2.5 HAEs) are
within cycle-1 ALMA field.
z=2.2 HAE
5
0
-5
R.A. [arcmin]
Dec. [arcmin]
4
the kinematic of ionized gas
5
T h e K M O S K i n e Sm o
a b t r i ac l S e u t r av le . y o
f z ⇠ 1 G a la x ie s
0
z=2.5 HAE
5
0
R.A. [arcmin]
-5
Sobral et al., submitted
Other emitters in SXDF
Dec. [arcmin]
Dec. [arcmin]
[OII] emitters at z=1.5-1.7
0
0
z=2.2 HAE
5
0
-5
Dec. [arcmin]
R.A. [arcmin]
5
0
-5
R.A. [arcmin]
blue: z=1.47 traced by NB921 (Ouchi+09,10, Sobral+12)
green: z=1.62 traced by NB973 (Ota+10, Tadaki+12)
red: z=1.69 traced by NB1006 (Shibuya+12, Tadaki+)
0
(z=1.2 traced by NB816,Yuma+13)
z=2.5 HAE
5
0
R.A. [arcmin]
-5
Other emitters in SXDF
Dec. [arcmin]
Dec. [arcmin]
[OIII] emitters at z=3.2
0
0
z=2.2 HAE
5
0
-5
Dec. [arcmin]
R.A. [arcmin]
z=2.5 HAE
0
R.A. [arcmin]
0
R.A. [arcmin]
0
5
5
-5
-5
Other emitters in SXDF
redshift
tracer
reference
~1.5
Hα
Yabe+12
2.2
Hα
Tadaki+13
2.5
Hα
Tadaki+13
3.2
[OIII]
-
1.2
[OII]
Yuma+13
1.5
[OII]
-
1.6
[OII]
Tadaki+12
1.7
[OII]
-
2.2
Lyα
Nakajima+12
5.7
Lyα
Ouchi+08
6.6
Lyα
Ouchi+10
Dec. [arcmin]
Summary of Subaru emitters in SXDF
0
5
0
-5
R.A. [arcmin]
dust continuum
[CII] line
Band-7 and 6
blue: [OII] emitters at z=1.5-1.7
green: [OIII] emitters at z=3.2
red: Hα emtters at z=2.2, 2.5
complicated!
→we focus on Hα emitters or Lyα emitters.
dust continuum
[CII] line
Cycle-2 Survey
Extension of cycle-1 SXDF-ALMA survey (Kohno et al.)
different band
wide frequency
5σ=0.3mJy in cycle-1 survey
Band-6, Δν=7.5GHz in cycle-1 survey
deep
wide field
0.5″ in cycle-1 survey
higher resolution
100″×50″ in cycle-1 survey
Strategy
HUDF is the best field for ALMA deep survey.
When the survey area is larger than HUDF, SXDF-CANDELS field would be unique.
However, the survey area should be less than 10 arcmin2.
We need to add some extra value to cycle-2 survey!
how about a survey pointing Hα emitters?
Goal 1: detection of dust continuum from Hα emitters at z~2
Goal 2: unbiased survey of [CII] emitters at z~6
Extension to wide ﬁeld
Dec. [arcmin]
Patchy survey pointing Subaru emitters
0
5
0
-5
R.A. [arcmin]
blue: [OII] emitters at z=1.5-1.7
green: [OIII] emitters at z=3.2
red: Hα emtters at z=2.2, 2.5
Extension to frequency range and depth
3.4 hours in cycle 1 survey
↓×3
10.2 hours in cycle 2 survey
Dec. [arcmin]
Deep survey pointing cycle-1 ALMA field
0
5
cycle-1 data
0
-5
R.A. [arcmin]
275GHz
245GHz
1.875 × 2 = 3.75 GHz
3.75 × 8 = 30 GHz
1. dust continuum
deeper by a factor of two
5σ=0.3 mJy → 5σ=0.15mJy, corresponding to SFR ~ 50 M◉/yr
2. [CII] emitter survey
larger volume by a factor of four
→ z=5.90-6.74, this corresponds to a survey volume of 3×103Mpc3
Also, this can covers Lyα emitters at z=6.6
[CII] luminosity function
ALMA [C II] detections of SMGs in the ECDFS
1071
Swinbank+12c
1. limiting flux of this survey
6.25 min integration
→ 5σ=2mJy in Δν=200km/s
→ L[CII]=1.5×108 L◉ at z=6.3
2. number density of [CII] emitter
N(>L[CII]) ~ 103 Mpc
3. survey volume
z=5.90-6.74
→ ΔV= 3×103Mpc3
L[C II] /LFIR ratio as
function
of the
far-infrared are
luminosity
for our two
4.4detected!
ALMA SMGs compared to local star-forming galaxies and
Aafew
[CII]
emitters
expected
toz =
be
plot we also include the z = 4.76 LESS SMG from De Breuck et al. (2011; see also Coppin et al. 2009). We also include a number of
This is a very challenge observation.
rbursts and AGN from previous studies (Carral et al. 1994; Luhman et al. 1998, 2003; Colbert et al. 1999; Unger et al. 2000; Malhotra et al.
et al. 2005; Brauher et al. 2008; Stacey et al. 2010; Cox et al. 2011). For the local data, we calculate the median (dashed line) and scatter
re shows that the ratio
L[C IImore
high-redshift
ULIRGs
is a factor
of ∼10as
times
higher given their far-infrared luminosities compared
] /LFIR for
Allofthe
reason,
we
should
do this
well.
0. Right: the [C II] luminosity function at z = 4.4 from our survey compared to z = 0. For the z = 4.4 luminosity function, we assume that all
The main science should be a study of star-forming galaxies at z~2.
ting galaxies in the !z = 0.12 volume covered by our observations were detected and so we stress that these calculations yield only a lower
me density of high-redshift [C II] emitters. The z = 0 observations are derived from volume density of IRAS sources at z < 0.05 from Brauher
e red dotted line shows the predicted [C II] local luminosity function for a constant L[C II] /LFIR = 0.002, whilst the solid line shows the z = 0
Extension to frequency range and depth
Advantages in the case of deep survey pointing cycle-1 ALMA field
8
Tadaki et al.
M*-SFR diagram for HAEs at z~2
100-
Uncorrected
Corrected
10
10
2
cycle-1 ALMA data is unique
(but the data is not obtained yet...)
10
- HAE sample is unique
1we have the SFG sample with 50<SFR<100
1
10
100required
10001
10
100
1000
deeper
data is
SFRHα [Msolaryr-1 ]
SFRHα [Msolaryr-1 ]
Fig. 8.— Lef t: Hα-based SFRs (SFRHα ) versus UV-based
SFRs (SFR
) withoutdata
dust-correction
for the combined sample
UV
KMOS
is
unique
of HAEs at z = 2.2 and z = 2.5. Right: Same as the left panel,
but with the
dust
correction
basedyet...)
on the SED fitting.
(but
theextinction
data is not
obtained
SFRHα [Msolaryr-1 ]
SFRUV [Msolaryr-1 ]
1000
3
SFR=100M◉/yr
cycle-1
SFR=50
10
cycle-2
1
MIPS source
Best fit line
Daddi et al. 2007
where m1500 is the interpolated magnitude at the rest0
10
9
10
11
frame wavelength of 1500 ˚
A.
10
10
10
Tadaki+13a
The HAE surveys with NB filters allow us to measure
M * [Msolar]
the Hα fluxes from the flux densities in NB and BB,
hence SFRs for all galaxies (Koyama et al. 2010). The
Fig. 9.— Star formation rates of the combined sample of HAEs at
z = 2.2 (green) and z = 2.5 (blue) plotted against stellar masses.
NB flux density can be defined as fNB = fc + Fline /∆NB ,
dust continuum observations, thisWe
field
is Hα
superior
towith
HUDF.
use the
-based SFRs
the dust extinction correction
where fFor
c is the continuum flux density, Fline is the
(Section 4.3). The errors in SFRs are estimated from the photoemission-line
flux, andwe
∆ can
denotes
FWHMs an
of the
filMoreover,
conduct
unbiased
[CII]
emitter
aslinewell.
metric
errors
(σ = 1). survey
The red solid
indicates the best fit line
0.94
ters. The BB flux density is also defined as fBB =
to our data points (SFR=238M11 ). The dashed line presents the
fc + Fline /∆BB . Therefore, the line flux, continuum flux
main sequence of star-forming galaxies at z ∼ 2 defined by Daddi
et al. (2007). Magenta squares indicate the MIPS 24 µm-detected
Summary
5σ=0.3mJy in cycle-1 survey
↓
5σ=0.15mJy
deep
0.5″ in cycle-1 survey
↓
0.5″ for consistency’s sake?
higher resolution
different band
wide frequency
Band-6, Δν=7.5GHz in cycle-1 survey
↓
Band-6, Δν=30GHz
wide field
100″×50″ in cycle-1 survey
↓
same field
For my science case, higher resolution is desirable (0.15-0.2″).
I will talk about this in ALMA high-z/AGN work shop (28 Oct.)
Patchy survey pointing HAEs at z 2
In the case of concentrating on our KMOS targets
The KMOS sample consists of 22 HAEs at z=2.2 and at z=2.5.
The survey volume is 1.5×103Mpc3
0
z=2.2 HAE
5
0
-5
R.A. [arcmin]
Dec. [arcmin]
19 pointings in cycle-1 → 3.4 hours
17 pointings in cycle-2 → ~3 hours
(in the same depth as cycle-1 survey)
Dec. [arcmin]
Five out of 22 HAEs at z=2.5 will be observed by ALMA (cycle-1).
We observe 17 HAEs in cycle-2.
0
z=2.5 HAE
5
0
R.A. [arcmin]
-5
Patchy survey pointing LAEs at z=6.6
SXDF-CANDELS field or SXDF field
ALMA FoV
z=6.3 [CII] emitter
z=6.6 LAE
z=6.1 [CII] emitter
250GHz
z=6.6
biased survey
1.875 × 2 = 3.75 GHz
265GHz
dc~150Mpc
z=6.2
un-biased survey of [CII] emitters
We can target a [CII] line from Lyα emitters at z=6.6.
Moreover, we can conduct an unbiased [CII] emitter survey as well.