Strongly lensed high redshift galaxies identified in Herschel wide surveys
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Transcript of Strongly lensed high redshift galaxies identified in Herschel wide surveys
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Strongly lensed high redshift galaxies identified in Herschel wide surveys Prospects for ALMA observations
Alain Omont (IAP, CNRS and Université Paris 6)
On behalf of the H-ATLAS and HerMES Teams and the IRAM Team
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Strongly lensed high redshift galaxies identified in Herschel wide surveys Prospects for ALMA observations
Using gravitational magnification for studying Ultra-Luminous InfraRed Galaxies (ULIRGs) at high redshift
• Introduction - (Local ULIRGs) - High-z ULIRGs and the magic of the submm window - Mm/submm continuum & line studies of high-z ULIRGs: the promise of ALMA - Herschel wide surveys multiply by 100 the number of high-z ULIRGs identified - Herschel lenses increase the sensitivity by ~10 for studying high-z ULIRGs
• Herschel high-z strong lenses- Early studies of Herschel lenses- Prospects and Current status
• Example: H2O mm/submm lines at high z in Herschel lensed galaxies
• Examples of ALMA programs possible with Herschel high-z lensed galaxies
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Arp 220: prototype of ULIRGs • LIR = 1.4×1012 Lo • thought to be in the final stage of merging• radio & NIR imaging double nuclei projected separation ~300 pc• MH2 ~ 1010 Mo within central kpc in accord with simulations of galaxy mergers
M 82: prototype of LIRGs, • 3.2 1011 Lo• Strong mid-IR PAH emission, even in strong outflow• Most high-z ULIRGs seem to have IR SEDs similar to M 82
Arp 220 M 82
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ULIRGs observed with the WFPC2 of the HSTat optical wavelengths. Many of these ULIRGs are merging galaxies
See Steve Lord’ s talk
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SMGs: strongest starbursts in the UniverseImportant players of star formation at z >~ 2
ULIRGs are much more numerous at high redshift than locally factor close to 1000 at z=2
Revealed by SCUBA surveys at 850µm (+ MAMBO at 1.2mm AzTEC, LABOCA, BOLOCAM) « Sub-Millimeter Galaxies » (SMG)
Easy detection of dust FIR emission through « inverse K-correction », same flux observed at l ~ 1mm from z ~ 0.5 to 10
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from Bertoldi, Voss, WalterLFIR(Lo) = 4x1012 S1.2mm(mJy)
FIR emission of cold dust (Td ~ 30-40 K) :
- steep submm spectrum - compensates for distance - Sn practically independent of z from z ~ 0.5 to 10
Effect often known as « negative K correction »
Redshift degeneracy
Dust detection: The Magic of the high-z submm window
SPIRE
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ULIRGs and Star Formation at high-z• ULIRGs dominate star formation at z>~2• SMGs (and Herschel/SPIRE) sources are luminous ULIRGs They provide only a small fraction of total star formation
>ULIRGs > z=2 SMGs SPIRE sources
Lindner+ 2011 Le Floch+ 2005
1.2mm
Total
Spirals
LIRGsULIRGs
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SMGs: strongest starbursts in the UniverseImportant players of star formation at z >~ 2
Revealed by SCUBA surveys at 850µm (+ MAMBO at 1.2mm AzTEC, LABOCA, BOLOCAM) Easy detection of dust FIR emission through « inverse K-correction », same flux at ~1mm from z ~ 0.5 to 10
Giant starbursts at the peak of elliptical formation z ~ 2-3 1-4
A few 1012Lo: at least ULIRGs ~1 per 3-5 arcmin2
Most exceptional HLIRGs 1013Lo ~1 per 50-100 arcmin2
nothing equivalent in the local Universe probably in most massive DM halos progenitors of BCG/cD galaxies of clusters?
Only ~1000 SMGs provided by SCUBA/MAMBOASTEC/BOLOCAM surveys ( <~ 1-2 deg2)
Herschel surveys are detecting several 105 SMGs
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IRAM-PdBI
Mm/submm studies of high-z ULIRGs
- High extinction makes optical/NIR studies of high-z ULIRGs hardly feasible- Extinction is practically negligible in mm
In addition to continuum, molecular mm lines are key tool for high-z ULIRG studies
CO lines are the strongest and most important (but C+):They give the mass of molecular gas MH2
(Rotation) velocity profileSpatial extension of molecular gas dynamical massRotation line ladder (SLED) TK + nH2 multi-TK gas
AGN excitation of high-J lines HCN is the best tracer of dense gas and star formation
H2O traces warm, dense gas and very strong IR
C+ (very strong, very high freq.) traces diffuse, (partially) ionized gas
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IRAM-PdBIIn addition to continuum, molecular mm lines are key tool for high-z ULIRG studies
CO lines are the strongest and most important (but C+):They give the mass of molecular gas MH2
(Rotation) velocity profileSpatial extension of molecular gas dynamical massRotation line ladder (SLED) TK + nH2 multi-TK gas
AGN excitation of high-J lines HCN is the best tracer of dense gas and star formation H2O traces warm, dense gas and very strong IR C+ (very strong, very high freq.) traces diffuse, (partially) ionized gas
ALMA
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PdBI CO high-resolution study of SMGSTacconi et al. 2008
Compact post-merger Resolved pre-merger
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HERSCHELSee Steve Lord’ s talk
Space Observatory, ESA (+NASA)
3.5m dish
3 instruments:5
• Camera-photometer, FTS- SPIRE 250-500µm wide surveys 1000 deg2
~4 x 105 high-z ULIRGs- PACS 70-160µm
• Heterodyne- HIFI
May 2009 January-March 2013
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Herschel high-z extragalactic wide surveys
H-ATLAS 550 deg2
HerMES 70 deg2 deeper + 270 deg2 shallow
Both mostly SPIRE (250, 350, 500µm) close to confusion limit
Plus • PACS surveys: smaller areas, deeper• HLS: lensing clusters,• 100 deg2 overlap with SPT (South Pole Telescope)• AKARI/NEP ?• etc.
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H-ATLASPIs Eales & Dunne
550deg2
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The HerMES surveySPIRE Guaranteed Time; PIs Seb Oliver & Jamie Bock
~900h (Multi-level Deep fields ~5 deg2 )
Wide fields
• ~70 deg2 Practically all Spitzer wide fields: SWIRE (Lockman, ELAIS-N1, ELAIS-N2, XMM-LSS, CFDS, ELAIS-S1) + FLS, Bootes, AKARI-ADFS
• practically all observed • mostly SPIRE (250, 350, 500µm) practically at the confusion limit
• somewhat deeper than H-ATLAS multi-l ancillary data
+ HeLMS 270 deg2 shallow, equatorial, RA ~ 0
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without optical IDs with optical IDsHerschel surveys revolutionize
the field of high-z submm galaxies
Several 105s high-z sources
Half H-ATLAS sources have z>1(inverse K-correction)
All high-z sources are ULIRGswith SFR > 300 Mo/yr
and LFIR > 1012 Lo
Some Herschel/SPIRE sources are warmer than SMGs and not detected at ~1mm
Some cold SMGs not detected by Herschel
Lapi et al. 2011
Lapi et al. 2011
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Herschel lenses increase the sensitivity by ~10 for studying high-z ULIRGs
The power of gravitational lensing
Since 20 years lenses mark the frontier of mm radioastronomy
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Gravitational lensing
« Einstein Cross » Einstein ring QSO (radiogalaxy) Cloverleaf QSO
X-Ray optical
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Unlensed SMGS Neri+ 2003
Lensed Cloverleaf
Thanks to magnification factor µ ~11- CO lines are more intense by ~10 than in unlensed SMGs- High S/N HCN & HCO+ lines are detectedwhile they are out of reach in unlensed SMGs with current PdBI sensitivity
The power of gravitational lensing
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Cloverleaf
The power of gravitational lensingSince 20 years lenses mark the frontier of mm radioastronomyRowan-Robinson’s galaxy
FIRAS10214 Swinbank’s Eyelash SMMJ2135
APM08279+5255
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Herschel lenses increase the sensitivity by ~10 for studying high-z ULIRGs
Herschel high-z strong lenses
Early studies of Herschel lenses
Prospects and Current status
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Negrello et al. 2010
Submm wide surveys are ideal for finding high-z lenses
- High-z submm sources are very strong (‘inverse K-correction’)
- Very steep unlensed counts
Almost half of the strongestSPIRE sources are high-zlenses
Very easy to identifyfrom local galaxies (+ blazars)
radio
unlensed
lensed
Local galaxies
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(faint)
Early studies of Herschel high-z strong lenses
1. H-ATLAS SDP Field Negrello et al. Science 2010
~14.4 deg2 7000 sources
Brightest 500µm sources:11 sources with S500μm > 100 mJy4 nearby galaxies (z<0.05), + 1 blazar, 1 galactic blob
5 high z candidates confirmed redshifts z = 1.5 – 3.4
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SED of lens candidates in H-ATLAS S DP fieldclear cases of double-source SEDs
z~0.2-0.8 elliptical galaxy + high-z ULIRG
Negrello+2010
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ID15.141
Submm photometric redshiftsRatios S250/S350 & S350/S500
plus a template such as Arp220 submm z-phot
Good agreement with zCO
for 6 sources with zCO
A good value of z-phot is important for searching zCO
with a limited bandwidthAdding 1.2mm MAMBO flux helps: S1.2mm=10-40mJyDannerbauer+
Measuring zCO at z>~4 is difficult with Zspec, impossible with Zpectrometer PdBI, EMIR or CARMA blind searche.g. ID15.141
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Zspec Lupu et al. to be submitted to ApJ
Redshifts have been confirmed with PdBI or CARMA interferometers
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Best, highest-z H-ATLAS SDP lenses
Sub-Millimeter Array images at 870µmExtended images: gravitational arcs on top of the lens galaxy
Red 870µm contours on top of I Keck image
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Extended images: gravitational arcs on top of the lens galaxy
from Negrello ESLAB2010
Idealized gravitational arcs
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S. Serjeant
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(faint)
Early studies of Herschel high-z strong lenses
2. H-ATLAS prominent z=4 lens ID15.141 Cox et al. 2011
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Z = 4.24
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(faint)
Early studies of Herschel high-z strong lenses
3. HerMES SDP exceptional lens
HerMES Lockman-01 = HLSW-01Very wide image
Riechers et al. 2011 PdBI, SMA & CARMA mapsK. Scott et al. 2011 Z-Spec spectroscopyGavazzi et al. 2011 lensing modeling
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HerMES Lockman-01 = HLSW-01 PdBI + SMA Riechers+ 2011
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Prospects for studies of Herschel high-z strong lenses
• A simple extrapolation of 5 lenses in 15 deg2 H-ATLAS SDP yields ~200-300 similar lenses in total in ~1000 deg2 Herschel surveys
• This number may be much increased by lowering the flux limits, e.g. by a factor >~5 for S(350µm) > 80 mJy
• Work is in progress for extensions of lens identifications:- larger areas- lower flux limits- use of additional data, e.g. NIR surveys for identifying the
deflectors
• One may thus expect thousands of Herschel high z lenses,including ~50-100 lensed sources in which the magnification is > 10
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Prospects for studies of Herschel high-z strong lenses
The two main applications of Herschel lenses should be:
1. Deep studies of high-z lensed sources (see below e.g. for H2O, ALMA )
2. Studying the evolution of dark matter halo of the deflectors - Most deflectors are massive spheroids with a few spirals and groups
- Redshifts of the deflectors are found mostly between z = 0.2 and 1, with a significant fraction at z>1. This is much higher than for the deflectors of optical lenses
- A major goal is thus to check the evolution of dark-matter halos at z~ 1
In addition Herschel wide surveys are important tools for cosmological studies, through map fluctuation studies, etc. (see e.g. Cooray+ 2010)
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Work in progress on Herschel high-z strong lenses
Enormous amount of work for identifying and following up hundreds of Herschel lenses
2/3 of observations carried on; half of them well processed
Several hundreds: identified candidates planned HST snapshots
Several tens: 1mm observations PdBI next Winter CO redshifts PdBI next Winter Identifications of deflector candidate with z-phot
About 10: High-resolution mm/submm images PdBI next Winter High-resolution optical/NIR (HST, Keck-AO…)
Spectroscopic redshifts of deflectorLens models
About 5: Other lines than CO (and CI): H2O, C+ PdBI next Winter
Multi-line CO SLED IRAM-30m next Winter
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H2O mm/submm lines at high z
- Strong H2O emission in the nuclei of local ULIRGs
- H2O in high-z lensed QSOs
- H2O in Herschel lenses
- Prospects
H2O is one of the most abundant molecules in the ISM
- In cold clouds practically all in ice on grainsabundance up to ~10-4, 1/3 of total oxygen
- Desorbed into the gas in hot cores
No confirmed detection of H2O at high z prior to 2011
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H2O in local ULIRGs (Mrk 231)
H2O is one of the most abundant molecules in the ISM
- In cold clouds practically all in ice on grains abundance up to ~10-4, 1/3 of total oxygen - Desorbed into the gas in hot cores
But it is very difficult to observe in the gas:
- Needs to be desorbed from the grains - At low z: H2O lines are completely absorbed by water in the Earth atmosphere space - At high z: H2O lines are very weak without lensing amplification
No confirmed detection of H2O at high z prior to 2011
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Strong H2O emission in the nuclei of local ULIRGsCompact single- double-nuclei (+AGN) of major mergers
see talks by D. Sanders and others
Prominent FIR H2O absorption lines in local ULIRGs (+AGN) such as Arp220 , Mrk231… (ISO; Herschel Gonzalez-Alfonso +2011)
Evidence for high H2O abundance from H218O , and high 18O/16O ratio
(Gonzalez-Alfonso+2011, Martin+2011)
Herschel/SPIRE: spectacular submm emission linese.g. Mrk231 (obscured QSO) (van der Werf+ 2010) - Several H2O lines up to Eexc~600K- Strong lines comparable to CO (very different from M82 and PDR)- Plus high-J CO (strong), [CI], H2O+, OH+, HF, CH+, [NII], etc.
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Van der Werf et al. 2010
GHz
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Gonzalez-Alfonso+ 2010
SPIRE van der Werf+ 2010
CO J 15 14 13 12 11 10 9 8 7
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Strong H2O emission in the nuclei of Mrk 231
Prominent FIR H2O absorption lines in local ULIRGs (+AGN):Arp220, Mrk231 Evidence for high H2O abundance from H2
18O , and high 18O/16O ratio
Herschel /SPIRE: spectacular submm emission linese.g. Mrk231 (van der Werf+ 2010) - Several H2O lines up to Eexc~500K, - Strong lines comparable to CO (very different from M82)- Plus high-J CO, [CI], H2O+, OH+, HF, CH+, [NII], etc.
Implications (Gonzalez-Alfonso+ 2010):- Lower levels may be excited by warm dense gas (~100K, ~106cm-3), with high H2O abundance (>~10-6)
- Higher levels imply intense FIR excitation in few 100s pc- Possible role of shocks, AGN (XDR), CR excitation, but unclear
High z: Many objects similar to MrK231 are expected, but very few detections of H2O are reported up to now Herschel lenses
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H2O lines must be easily detectable in many Herschel lenses
• Herschel SPIRE 250/350/500 µm surveys (~1000deg2) are ideal to find rare, high-z strongly lensed SMGs Negrello+2010 • Only 1-2 deg2 observed by ‘traditional’ SCUBA/MAMBO/ASTEC surveys practically no strong lens
• Breakthrough by Herschel surveys hundreds of strong high-z lenses (while only ~6 found before Herschel)
• Unique opportunity for deep studies of high-z mm/submm linesAs performed with classical mmlenses, e.g. the Cloverleaf
• H2O line intensities are a significant fraction of that of CO lines in Mrk 231. They should be easily detectable in strongly lensed similar high-z ULIRGs
Negrello+ 2010
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PdBI detection of H2O in H-ATLAS SPD-17b z = 2.305
ZSpec H2O tentative detectionLupu et al. 2011
H-ATLAS SPD-17 identified as lensed ULIRG by Negrello+ 2010Complex HST image (Negrello+ in prep.)Rich spectrum: high-J CO z=2.308 Lapp~4 1013LoPossible H2O 202-111 at 299GHz: seems very strong but noisy (2.6s)
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PdBI detection of SPD-17b at 299GHz z=2.3Omont et al. 2011 A&A 530, L3
GHz
km/s
Compact D-conf.
Continuum 32+/-2 mJy
(+ extended A,B Confs.not yet fully processed)
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Detection of H2O in H-ATLAS G12-29 z= 3.3One of the strongest Herschel lensed sources: S500µm = 285 mJy, even detected by Planck
Z-Spec/APEX spectrum (Lupu+ in prep.) impressive high-J CO lines up J=10-9 (11-10?) z~3.254 Confirmed with Zpectrometer 3.2588±0.0012
Strong line at 273.3GHz H2O 321-312
needed to be confirmed
273 GHz is not currently observable with PdBI, but another strong H2O line is expected at 231.96 GHz (in a bad ZSpec channel)
(H2O is also tentatively detected at 257.7GHz)
PdBI Detection of H2O 202-111Preliminary results (R. Neri)
• C-conf., 6 antennas• Very robust detection
• I ~ 5 +/-0.55 Jy.km/s ~ I(SPD.17b) / 2 ~same luminosity
• 231.96 GHz z = 3.260• Width 680 km/s
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Lensed images of G12-29
Multi-galaxy deflector
The K image is very different from ~1mm images
Keck K-band SMA 870µm PdBI 1.3mm continuum + H2O
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5 other detections of H2O in high-z sources(at IRAM 2011, except Cloverleaf)
• Multi-line detection in the lensed QSO APM08279+5255 z = 3.9 van der Werf et al. 2011, plus Lis et al. 2011, Bradford et al. 2011
• Zspec tentative detection in the lensed QSO Cloverleaf z= 2.56 Bradford et al. 2009
• Plus recent detections of two other Herschel sources and one QSO
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Inferred conclusions for H2O in high-z ULIRGs
The detection of H2O implies special excitation conditions in an intense IR field and a warm dense gas, similar to Mrk 231 with higher luminosity
The high H2O/CO ratio makes it unlikely that the H2O emission originates in classical PDRs
But all the evidence suggests that SDP.17b, G12-29 and Mrk 231 have similar properties, with warm, dense gas and strong IR field ( plus possibly shocks, XDR, CR).
However, this needs to be confirmed by higher excitation lines of H2O ALMA
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Prospects for H2O studies in Herschel lenses (with ALMA)
(Full) ALMA will easily detect H2O multi-lines in hundreds of Herschel high-z lenses (filler in ALMA Cycle 0 for 3 sources, and search for H2O in 8 additional H-ATLAS lenses is scheduled at 18 PdBI next Winter)
Together with high-J CO lines, H2O lines will provide rich information about the conditions in the dense warm ISM of the compact merger nucleiof SMGs, and their strong FIR, plus shocks, X Rays, Cosmic Rays, etc.
The full ALMA sensitivity will also allow detection of weaker lines or details of H2O lines such as:
- Absorption lines - Outflows - Isotopologues H2
18O, H217O (possibly HDO, D2O?)
- Other molecules detected in Mrk 231: OH+, H2O+ (related to H2O and allowing diagnostic of XDR chemistry), HF, etc. - And many other molecules allowing, together with H2O, further checks of the ISM of merger nuclei for their physical conditions, chemistry, dynamics, AGN influence, etc.
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ALMA
50 x 12m dishes+ ACA array 7m dishes
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Prospects, strategy and questions for ALMA• There will be 100’s of strongly lensed sources available for ALMA - Object selection in function of goals
- Systematic studies of specific classes if populated enough
- Muli-l studies: EVLA, JWST, HST, etc.
This would allow in particular to populate rare classes of objects for comprehensive ALMA studies, e.g.
- highest redshifts, z>4 even z>5 - strong AGN of various types - radio loud - LIR> 1013Lo, LIR<1012Lo - H2O mega-masers - cluster lensing - extremely strong amplification, etc.
• Studies of the lensing galaxies through ALMA observations will have important cosmological applications
But detailed lensing models are needed for inferring properties of lensed SMGs
• Anyway, ALMA will have a fantastic time with such sources!
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Examples of ALMA programs possible with Herschel lenses
• Blind CO redshift determination and the highest redshifts - Finding redshifts for 100’s sources remain a major issue
- Searching for z~>~6 objects (lensed or not) is specially important
• ALMA high-resolution imaging of strong lenses - ALMA can do that in the continuum, CO lines & C+line (+H2O lines, etc.)
- Structure of the ISM and SF; AGN molecular torus - Dynamics: rotation, Mdyn, mergers, outflows, etc.
• High sensitivity molecular (and atomic) spectroscopy - H2O, HCN...: diagnostic
- etc.: chemistry, isotopologues
• Golden objects with two background sources lensed by the same galaxy, making possible cosmological tests that are independent of the mass of the lens.
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ALMA Cycle 0 Projectson Herschel high-z strongly lensed galaxies
Accepted (top 10%)
- 0.53’’ resolution snapshot mapping at 870µm of30 HerMES lenses (Riechers et al.)
- Comprehensive study of a z=1 H-ATLAS lens (Orellana et al.)
Fillers- Multi-line H2O study in the three high-z H2Osources visible from ALMA (van der Werf et al.)- Dense gas tracers (HCN,HCO+ …) in H-ATLAS SDP sources (Lupu et al.)- High-resolution mapping of a cluster-lensed high-z source(Egami et al.)
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Summary
• Herschel surveys will observe ~1000 deg2
• First lens identifications and intensive follow-up confirm that one may expect hundreds of lensed SMGs with magnification ~5-10
Unique legacy for mm/submm studies of molecular gas in high-z major starbursts (ULIRGs even below the confusion limit)
• Effective sensitivity increase by ~10 for ALMA, IRAM/NOEMA etc. for studies of high-z ULIRGs
• H2O is an important tracer of compact, dense warm, strong-IR nuclei of SMGs, especially obscured AGN
• New step in studying high-z lensing and their dark matter structures at higher deflector redshift up to z >~ 1
• But needs much follow-up and high-quality lensing modeling