wide-field hi galaxy surveys the arecibo legacy fast alfa (alfalfa) survey and its predictions for...
TRANSCRIPT
Wide-Field HI Galaxy SurveysThe Arecibo Legacy Fast ALFA (ALFALFA)
Survey and its Predictions for Future Surveys
Martha HaynesCornell University
STScI13 June 2011
ALFA is not a car…
ALFA is not a car…
Arecibo L-band Feed Array (ALFA)
It is a radio “camera”
Arecibo L-band Feed Array (ALFA)
It is a radio “camera”
ALFA is not a car…
Arecibo L-band Feed Array (ALFA)
It is a radio “camera”
• An extragalactic spectral line survey • To cover 7000 sq deg of high galactic latitude sky• 1345-1435 MHz (-2000 to +17500 km/s for HI line) • 5 km/s resolution• 2-pass, drift mode (total int. time per beam ~ 40 sec)• ~2.3 mJy rms (at 10 km/s resolution)
=> MHI~105 M in LG, ~107 at Virgo• 4400 hrs of telescope time, 5+ years (actual completion fall
2012)• Highly efficient: 99% “open shutter” time• Oversees acquisition of TOGS (galactic HI) data• Started Feb‘05; as of Apr’11, 92% complete (741 observing runs)
=> ALFALFA 40% catalog: 15000+ detections covering a cosmologically significant volume at z=0
• One of several major surveys currently ongoing at Arecibo, exploiting its multibeam capability
http://egg.astro.cornell.edu/alfalfa
ALFALFA, a Legacy Survey
http://egg.astro.cornell.edu/alfalfa
ALFALFA, a Legacy Survey
Check out the ALFALFA blog!
•ALFA beams are 3.3’x3.8’
•“Almost” fixed azimuth drift mode
•2nd pass offset from the first to give 1.05’ sampling
“Minimum intrusion”99% open shutter time
•ALFA beams are 3.3’x3.8’
•“Almost” fixed azimuth drift mode
•2nd pass offset from the first to give 1.05’ sampling
•ALFA beams are 3.3’x3.8’
•“Almost” fixed azimuth drift mode
•2nd pass offset from the first to give 1.05’ sampling
“Minimum intrusion”99% open shutter time
•ALFA beams are 3.3’x3.8’
•“Almost” fixed azimuth drift mode
•2nd pass offset from the first to give 1.05’ samplingALFALFA survey strategy:
Keep it simple! “Minimum intrusion”99% open shutter time
•ALFA beams are 3.3’x3.8’
•“Almost” fixed azimuth drift mode
•2nd pass offset from the first to give 1.05’ samplingALFALFA survey strategy:
Keep it simple! “Minimum intrusion”99% open shutter time
The ALFALFA team: An open collaboration
Riccardo Giovanelli PI
Heavy student involvement:
• 6 PhDs to date• 11 PhDs underway• 125+ undergrads• Dozens of undergrad
thesis projects
Undergrad ALFALFA team
39 papers in refereed literature (appeared or submitted)
No full-time professional staff
1. Census of HI in the Local Universe over cosmologically significant volume
2. Determination of the faint end of the HI Mass Function and the abundance of low mass gas rich halos
3. Environmental variation in the HI Mass Function
4. Blind survey for HI tidal remnants
5. Determination of the HI Diameter Function
6. The low HI column density environment of galaxies
7. The nature of HVC’s around the MW (and beyond?)
8. HI absorbers and the link to Ly absorbers
9. OH Megamasers at intermediate redshift 0.16 < z < 0.25
ALFALFA Science Goals
HIPASS completeness limit HIPASS detection limit
HIPASS bandwidth edge•ALFALFA covers adequate volume with adequate sensitivity
• 15000+ detections• 70% are “new”
Important advantages:
•In addition to sensitivity, bandwidth and velocity resolution, ALFALFA yields positions to < 20”
Identify most probable optical counterpart (OC)
• Continuum/RFI tracked Allows stacking at
arbitrary positions
ALFALFA 40% catalog
Lowest mass systems:•detected only nearby•narrow velocity widths
FAA radar
.40 sampleHaynes+2011
FAA harmonic +GPS/NUDET
Virgo
Haynes+ 2011 (about to be submitted)
Mining ALFALFASignal extraction done in Fourier domain using matched filter algorithm (Saintonge 2007, AJ, 133, 2087 )HI flux density sensitivity depends on emission width => but well-behaved
Amélie Saintonge PhD thesis
Gridview (Brian Kent)
Sources found by the signal extractor are examined interactively.• “Weight” at each 3-d grid point
accounts for “missing” data (RFI)• Polarization match checked (RFI)• Continuum map retained• Optical field
Multiwavelength applications
Fabello+ 2011 MNRAS (in press)
ALFALFA pipeline tracks RFI/continuum => Spectral stacking
to dig deeper
Silvia Fabello PhD thesis
Centroiding to <18”> (depends on S/N)Optical images (SDSS, DSS2B) and databases (NED, AGC) examined along with HI field
Most probable OC SDSS Photo/SpectObjIDs “Priors” (lower S/N; same cz) Extensive notes
Identifying Optical Counterparts
ALFALFA source centroids good to ~18” (depends on S/N)
ALFALFA catalogs include: • the HI centroid position• the position of the most
probable OC• OC’s SDSS PhotoObjID
and SpecObjID (where applicable)
Of 15855 sources in α.40:• 1013 have no OC• 844 of those could be
HVCs (or LG minihalos)• 199 (<2%) extragalactic• Of those, <50 are
“isolated”
4 tile centered at
+26
• 7000 sqd of high galactic latitude sky with median cz ~8800 km/s
• Undersamples clusters but traces well the lower density regions
• Large overlapping areas with SDSS and GALEX
Red: SDSSBlue: ALFALFA
Inner zone
Full bandpass
“Dark” object in a group
ALFALFA HI on SDSS r
HI peak with no/marginal optical UV: almost dark?
MH, RG (CU), John Cannon (Macalester), John Salzer (Indiana)
HI-selected galaxies
• Gas-dominated systems fill the blue cloud; but some gas-rich massive red spirals
• GALEX-Arecibo-SDSS Survey (GASS: Catinella+ 2010; Schiminovich+2010) and COLDGASS (IRAM30m: Saintonge+2011a,b) => scaling relations for massive galaxies (ALFALFA detects about 30% of GASS targets)
• High gas fraction massive HI disks: HIghMASS (colored symbols: stay tuned…)
SED fitting (SDSS+GALEX)
Shan Huang PhD thesis
HIMF from ALFALFA: Good news for the SKA!
HIPASS: Zwaan+2005
.40: Martin+2010
N=10119
N=4315
HIPASS: Zwaan+ 2005• Did not sample low/high mass ends• Issues of confusion in 15.5’ beam• Error bars are large!
Survey design must overcome cosmic variance and instrumental/selection bias
ALFALFA is the first blind HI survey to cover adequate volume at both the low and high HI mass ends
Martin+ 2010 ApJ 723, 1359• Based on contiguous regions in Virgo vs
anti-Virgo directions (35% of total)• 10,119 Code 1 (“best”); cz < 15,000 km/s• ΩHI = 4.3 ± 0.3 x 10-4 (16% higher than
HIPASS)
Ann MartinPhD thesis
HIghMass: High HI mass, gas-rich galaxies at z~0
ALFALFA detects a rich population with log MHI > 10.
• Candidates to migrate from BC to RS but not yet reached phase of significant SF?
• Alternative mode of (late) accretion?
=> higher than average spin parameter?
HIghMass: High HI mass, gas-rich galaxies at z~0
GALEX FUV
GMRT
Preliminary; Chengalur+
=> HI velocity field
ALFALFA detects a rich population with log MHI > 10.
• Candidates to migrate from BC to RS but not yet reached phase of significant SF?
• Alternative mode of (late) accretion?
=> higher than average spin parameter?
Shan Huang (PhD: GALEX, H, SED-fitting) Betsey Adams (PhD: GMRT/WSRT)
Greg Hallenbeck (PhD:EVLA)
Where are the dwarfs?
Papastergis+ ApJ (in press)
astro-ph/1106.0710
ALFALFA Velocity Width Function
(WF)
(to 20 km/s)
Are the low mass DM halos just
“missing baryons”?
“Bolshoi”
Manolis PapastergisPhD thesis
Baryon fractions as fn of halo mass
Simulations of different resolution;
lowest = filled circles;
highest = unfilled squares.
Hoeft et al 2006: Can small halos retain any baryons?
Ricotti (2009): Can gas accretion be reactivated at late z?
Leo T has 2.8x105 M of HI => prototype
Can we observe the threshold of baryon dropoff?
Low HI mass dwarfs: on the brink of extinction?
• FIGGS (Begum +): <log MHI> ~ 7.78
• Little THINGS (Hunter +): <log MHI> ~ 7.97
• Leo T: log MHI = 5.44SHIELD:EVLA BCD 2010-2011 => 180 hours
• John Cannon (PI); Betsey Adams (grad)
12 galaxies with <log MHI> ~ 6.7•Resolve HI => SF?•Trace DM halo
Hoeft+ 2006
Leo T as nearby prototype: outside MW virial radius (dist~420 kpc)
We have found a subset of the HVC phenomenon that appears to be compatible with the LG minihalo hypothesis (Giovanelli+ 2010, ApJL 708,L22)
**much** smaller than the Blitz et al. and Braun&Burton CHVCsMHI ~ 3 x 105 M; size ~ 0.7 kpc
Do not violate astrophysical constraints (Sternberg+ 2002)
Other interpretations are possible; we have not proved that the candidates are LG minihalos, but that remains a tantalizing possibility.
ALFALFA UltraCompact HVCs: LG Minihalos?
On-going work (Betsey Adams, RG, MH, J.Salzer)•Optimize signal extraction algorithm => ALFALFA CHVC catalog
•HI mapping: HI distribution, dynamics•Distances:
•TRGB (resolved CMDs)•H: ionized by galactic RF places lower limit
2.8x105 MM/L > 50
Ryan-Weber+
2007
Betsey AdamsPhD thesis
ALFALFA: Volume + Sensitivity•ALFALFA is the first blind HI survey to sample a cosmologically
significant volume at z=0 • Robust determination of HIMF at z=0• Work on ζ(r), VF and environmental variations on-going
•There are no “dark” HI galaxies with HI masses > 109 M
•ALFALFA sources provide the means to determine the baryon fraction as fn. of halo mass and test models of dropoff at Mhalo ~ 109 M
•ALFALFA identifies a set of gas-rich Local Group “minihalo” candidates; evidence which will refute or confirm that hypothesis is being sought.
•ALFALFA detects a previously-unrecognized population of very high HI mass galaxies with HI masses > 1010 M; in some, cool gas contributes the dominant form of baryons. => Good news for SKA!
•There is more ALFALFA to be harvested!
Future of Wide Area HI Surveys
• HI surveys are much less mature than OIR surveys
• But understanding the gas is important!
• HI selected samples very different from OIR selected surveys => star forming galaxies!
Wish list:• Deep survey of nearby grounds (sev hundred sqd) for Leo
Ts• Wide area survey (~SDSS volume) with <10” angular
resolution• Deep surveys at higher cz• Low column density diffuse HI surveys• (BAO/Intensity mapping; HERA experiments)
Technology advances will enable all this...
HI emission: simple but not easyHI 21 cm line: τ ~ 10 Myr (3 x 1014 sec)
• 1 Mʘ = 2 x 1014 g => 1.2 x 1014 atoms of HI• Total HI gas (“normal”) = log [7-10]• HI emission ~ 4 x 1049 to 4 x 1052 photons per sec• L(HI 21 cm) ~ 4 x 1033 to 4 x 1036 ergs s-1
For comparison, in SF galaxies:• L(Hα) ~ 3 x 1039 to 3 x 1042 ergs s-1
RFI from satellites:• Antenna arrays less affected if
frontend not saturated• But no protected regions
Arrays (antenna arrays, phased array feeds) present huge challenges:
• Required computations/datasets
• Electrical power requirements
HI 21 cm emission ~ 106 X less power than Hα
GPS NUDET
2-d (freq vs time) “drift”
Future of Wide Area HI SurveysWALLABY (ASKAP) + WNSHS (APERTIF/WSRT)
• Uncooled 37-beam PAF• Full sky survey out to z = 0.26• Resolution of 30” (maybe 10”) => where the gas is!• 0.7 mJy/beam (per 50 km/s channel) • 500,000 galaxies• e.g. WALLABY: 9600 hours (1200 points X 8hr)
A hunt for low mass halos (LeoTs) with AO40:• Cooled 40-beam PAF• 10X ALFALFA sensitivity: 0.3 mJy/beam (per 5 km/s
channel)• 300 sqd over nearest groups (CVn, NGC 628/672/784)• 1000+ hours
Diffuse HI (log NHI=17) survey with (clean beam) GBT• Limits on column density of gas (on 9’ scale)• See Jay Lockman’s poster
HI at higher redshiftDetecting HI emission is really tough
• Single galaxy at z = 0.176 (Zwaan+ 2001; WSRT 200 hrs)• Single galaxy at z = 0.189 (Verheijen+ 2004; VLA 80 hrs)• Two clusters at z=0.188 and 0.206 (Verheijen+ 2007;WSRT 420 hrs)
42 galaxies detected with log MH: [9.7-10.6]• 26 (of 33) with z= [0.17 to 0.25] (Catinella+ 2008; Arecibo 300 hrs)
SKA pathfinders will make first foray into statistical studiese.g. LADUMA on MeerKAT: (Baker/Blyth/Holwerda PIs)
• 5000 hours on EXDFS• Stacking at (pos,z) of known galaxies (few individual
galaxies detected)
But… real progress awaits full SKA sensitivity
HI surveys: summary• HI emission line surveys are hard! But they
yield important clues about cosmology and galaxy evolution (star forming galaxies!).
• ALFALFA is the first blind HI survey that samples a cosmologically significant volume with the required sensitivity, solid angle and velocity resolution• Robust measures of HIMF, ΩHI, ξHI, VFHI at
z=0 But it is limited in angular resolution (4’)
and z
• New array technologies (PAFs, antenna arrays) are enabling new capabilities => Lots to happen in the future!
19-beam PAF (NAIC/BYU) prototype for “AO40”
ASKAPMeerKAT
http://arecibo.tc.cornell.edu/hiarchivehttp://egg.astro.cornell.edu/alfalfa
ALFALFA sprouts!
•ALFA beams are 3.3’x3.8’
•“Almost” fixed azimuth drift mode
•2nd pass offset from the first to give 1.05’ samplingALFALFA survey strategy:
Keep it simple! “Minimum intrusion”99% open shutter time