Upload
esmond-gibbs
View
216
Download
0
Embed Size (px)
Citation preview
Emission Lines for BAO: Ground & Space
M. LamptonUCB SSL
1 Dec 2006Rewrites May 2007, Sept 2009, Nov 2009
M.Lampton Sept 2009 2
Intro
• Much previous BAO work has used LRGs: very bright! But few in number• Emission line galaxies are more numerous but not so bright• Star Formation Rate is gauged by emission lines esp Hα and [O II]• [O II] 3727 can accomplish a lot from mountaintops: 1 micron is z=1.68• Hα 6563 although stronger, requires spaceborne observatory• Then there’s [O III] 5007, yet another tool.
M.Lampton Sept 2009 3
Plan
1. BAO Goals: nP ~ 1 and lots of modes
2. Review SFR(z) and model it
3. Review LF(z) for Halpha and [O II]
4. Model LF(z) for Halpha and [O II]
5. Predict harvests of BAO surveys, space and ground.
Rough analogy to Parkinson et al “Optimizing BAO Surveys” arXiv 0702040 which was done to optimize WFMOS (ground only): they found it best to concentrate on 0.8<z<1.4 over the widest possible sky area and to kiss off Lyα at z~3.
Throughout: I adopt a “737” cosmology.
M.Lampton Sept 2009 4
Step 1: Uncertainties in the Acoustic Scale Lengthe.g. Blake et al 0510239 (2005); see also Reid et al 0907.1659
33-4
33-4
BAO
BAO
3
Mpc h 10P galaxies, blueFor
Mpc h102~ P galaxies, redFor
.0.2rad/Mpck rad/Mpc 0.07
with)P(kP and
Mpcper galaxiesn where
nP
11
Nmodes
1
X
X
Shot noiseCosmic varianceP(k) from Cole et al 2dFGRS arXiv 0501174, Fig.15
M.Lampton Sept 2009 5
Step 2: SFR, Hα, [O II] are strongly correlated
Local, SDSS: Sumiyoshi et al arXiv:0902.2064 (2009) Fig 3 Local; Kennicutt, Ap.J. 388, 310 (1992)
Hα 6563 singlet Sum of 3727, 3729
M.Lampton Sept 2009 7
Step 2: Review and model SFR(z)The Compilation:
Hopkins & Beacom ApJ 651, 142 (2006) Fig.1
The parabola:
log(SFR)=-2.00+5*(x – x2) where x=log(z+1)
See also Gonzales et al arXiv 0909.3517
M.Lampton Sept 2009 8
Step 3: LF data, Hα, continuedfaint end: Subaru; Ly et al., Subaru, ApJ 657 738 (2007), Fig 10
z=0.08 z=0.24
z=0.40
M.Lampton Sept 2009 9
HiZELS: a high redshift survey of Hα emitters. I: the cosmic star-formation rate and clustering at z = 2.23
J. E. Geach et al; UKIRT HiZELS: NIR narrowband at 2.12um, COSMOS field 0.6 sqdeg
arXiv:0805.2861v1
M.Lampton Sept 2009 10
MULTI-WAVELENGTH CONSTRAINTS ON THE COSMIC STAR FORMATION HISTORY FROM SPECTROSCOPY: THE REST-FRAME UV, H, AND INFRARED
LUMINOSITY FUNCTIONS AT REDSHIFTS 1.9<z < 3.41Reddy et al arXiv:0706.4091: 2000 SpectroZ, 15000 PhotoZ; Steidel Keck I w/ LRIS (2004)
M.Lampton Sept 2009 11
Step 3: LF data [O II]Ly et al., Subaru w/ narrowband filters; ApJ 657 738 (2007) Fig 12
z=0.89 z=0.91
z=1.19 z=1.47
M.Lampton Sept 2009 12
Step 3: LF data, [O II], continuedZhu et al., arXiv 0811.3035: DEEP2 (Keck II + DEIMOS), 14000 galaxies
M.Lampton Sept 2009 13
Step 3, continued: how about [O III] 5007?Ly et al., Subaru Deep Field; ApJ 657 738 (2007) Fig. 11
z=0.41 z=0.42
z=0.63 z=0.84
M.Lampton Sept 2009 14
Step 3 concluding:
LF compilationSumiyoshi et al:
Compilation based on data from SDF;
arXiv 0902.2064
Halpha [O II]
0.5<z<1.0
1.0<z<1.4
1.4<z<1.7
M.Lampton Sept 2009 15
Step 4: Model the LF(z) for each line
• Abell model (ARAA v.3, 1-22, 1965) parameters Lb, Nb at the break;
– Nearly flat power law at faint end
– Break
– Nearly inverse-square power law at bright end
• Schechter model (ApJ 203, 297-306, 1976) parameters L*, Φ* at the break;
– Nearly flat power law at faint end
– Break
– Exponential decrease at bright end
• Both developed for galaxy continuua
• They differ only at the bright end: Abell=slope; Schechter=dropoff.
• Which might apply for line emission?
• Because of the log-log straight-line LFs seen in DEEP2 (which go to very sparse densities) I adopt the Abell model here.
• Other adopters: Hao et al 0501042 (ELGs); Croom et al MNRAS 349 1397 2004 (QSOs) 1]N/N)2ln(exp[2
LL(N)
inverse... analytican has Abell Integral
LNln(2)
πLdL
dL
dN density Luminosity
)2ln(
)/LL1ln(NN
LL
LN
)2ln(
ln(10)
dLog(L)
dN
LL
LN
)2ln(
1
dLn(L)
dN
b
b
bb
22bb
L
22b
2bb
22b
2bb
Simplest Abell Luminosity Function
M.Lampton Sept 2009 16
Step 4: Hα LF modellog(Nb) = -3.5+2.0*(x-x²)
log(Lb) = +41.5+3.0*(x-x²)
where x = log10(1+z)
0.5<z<1.0
1.0<z<1.4
1.4<z<1.7
Sumiyoshi et al (2009)
M.Lampton Sept 2009 17
Step 4: [O II] LF modellog(Nb) = -3.5+2.0*(x-x²)
log(Lb) = +41.1+3.0*(x-x²)
where x = log10(1+z)
0.5<z<1.0
1.0<z<1.4
1.4<z<1.7
Sumiyoshi et al (2009)
M.Lampton Sept 2009 18
Step 4: [O II] modellog(Nb) = -3.5+2.0*(x-x²)
log(Lb) = +41.1+3.0*(x-x²)
DEEP2; Zhu et al., arXiv 0811.3035
M.Lampton Sept 2009 19
Step 5: Survey Yieldassumes “737” universe
microns2erg/sec.cm2
2
z
032
m
HC
L
2
22C
2L
P5.035E15hc
P sphotons/mF
redshiftz
cm 0.173z0.515z1
z1.325E28
)33(1
dyDD
distance luminosityD
erg/sec source, line theof luminosityL
.secerg/cm flux,power observedP
z)(14D
L
4D
LP
yyy
M.Lampton Sept 2009 20
For a given nP, what Hα flux do we expect?
This extrapolated LF based on Sumiyoshi has many uncertainties, and the JDEM BAO team has recommended a higher sensitivity, ~ 1.6E-16 erg/cm2s
NEWS FLASH : Previously sought nP=1 and Zmax=2; but Linder and others (this conference) recommend NP=2 or even 3; Zmax=1.7 not 2.0
Abell distribution eyeball fitted to Sumiyoshi et al 2009 Hα
M.Lampton Sept 2009 21
For a given nP, what [O II] flux do we expect?
Abell distribution eyeball fitted to Sumiyoshi et al 2009 [O II] 3727+3729
BigBOSS White Paper Fig.2 based on DEEP2 and VVDS
Goal: doublet flux ~ 1E-16 erg from this alone. But atmospheric observing complications and uncertainties about the LF at z>1.5 argue for higher sensitivity; working goal = 2.5E-17 erg/cm2sec for each component.
M.Lampton Sept 2009 22
A Telescope area for 3.8m Mayall 7.5 m²
Tobs Exposure time 1ksec to 4ksec
F Target line flux: 2.5E-17 erg/cm2s
Ta Atmosphere transmission GeminiZenith5mm1.414
Ts Spectrometer transmission 0.5
Q Sensor quantum efficiency 0.9
Bsky Brightness of sky √2 · GeminiZenith
Ωresol Solid angle, one fiber on sky 1.5 sq arcsec
Δλ Wavelength spanned by one fiber 2.8E-4 um
Nread RSS read noise pixels on one fiber 6 √44 =40 el
SNR Signal to noise ratio desired 8
QTTTA
NQTBTA
NQTBTA
QTTTA
saobs
readsresolobs
readsresolobs
saobs
2
2
SNRF
FSNR
BigBOSS
[O II] 3727,3729
Model MDLFs
M.Lampton Sept 2009 23
Atmospheric Transmission at Gemini Northpresumably similar at KPNO?
http://www.gemini.edu/sciops/ObsProcess/obsConstraints/ocTransSpectra.html
5.0mm H2O
U B V R I Z Y J H K
M.Lampton Sept 2009 24
Atmospheric Emissionhttp://www.gemini.edu/node/10781?q=node/10787#OpticalSkySpectrum
M.Lampton Sept 2009 25
MDLF Results for BigBOSSGoal is to use < 1 hour exposures and get SNR=8 (see chart 22)…
at z=2: 2.5E-17 erg/cm2s, will need the whole 4ksecat z=1: 1E-16 erg/cm2s, will need < 1 ksec
At Tobs = 1 h, 4000 fibers and 100 nights/year at 8h/night is 3 million targets per year -- and of course there is additional yield since most targets have z<2.0 and so won’t need the full 4000 seconds of exposure each,so smart fiber reallocation can improve yield rather than SNR.
M.Lampton Sept 2009 26
A Atelescope, 1.0m, 25% area obstructed 0.59 m²
Tobs Observing time per target 1000 sec
F Target line flux: 1.6E-16 erg/cm2s
Ts Spectrometer transmission 0.7
Q Sensor quantum efficiency 0.9
Bzodi Brightness of sky, ph/m2.sec.micron 2 · NEPzodi
Ωresol Solid angle, 2x2 pixels on sky 1.0 sq arcsec
Δλ Wavelength span seen by each pixel 0.7 microns
Nread RSS read noise for 2x2 pixels 8√4 = 16electrons
SNR Desired signal to noise ratio 6.0
QTTA
NQTBTA
NQTBTA
QTTA
sobs
readsresolzodiobs
readsresolzodiobs
sobs
2
2
SNRF
FSNR
JDEM, Hα 6563
Model MDLF
M.Lampton Sept 2009 27
MDLF Results for JDEM Goal is to use ~ 1ksec exposures Hα and get SNR>6…
at z=2: can get to 2.5E-16 erg/cm2s, using 1ksecat z=1: with 1ksec will gain improved SNR
At 1 kilosec exposures, 6 MCT sensors & 0.5 arcsec pixels, the FOV is 0.46 sq degrees. With 100 sec lost per maneuver and 70% on orbit efficiency, the net survey rate is 9000 square degrees per year.
M.Lampton Sept 2009 28
Recent Relevant Results!
• Geach et al “Empirical Halpha emitter count predictions for dark energy surveys” arXiv 0911.0686: ELGs, Ha, 0.5<z<2.
• Parkinson et al “Optimizing BAO surveys II: curvature, redshifts, and external datasets” arXiv 0905.3410
• Hutsi, “Power spectrum of the maxBCG sample: detection of AO using galaxy clusters” arXiv 0910.0492
• Stril et al, “Testing Standard Cosmology with Large Scale Structure” arXiv0910.1833; specifically compares BigBOSS vs JDEM-PS.
Conclusions
• JDEM-BAO: entirely feasible!
• BigBOSS: entirely feasible!