Matt Jarvis - Recent results from the Herschel-ATLAS

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  • 1. Recent results from the Herschel- ATLAS Matt Jarvis University of the Western Cape & University of Hertfordshire
  • 2. Herschel3.5m primaryLaunched in May 2009Continuum capabilities from70-550 microns
  • 3. The Cosmic IR background•  Contains as much energy asthe optical / UV background•  Half the energy emitted bystars and AGN since the BigBang has been absorbed bydust and re-emitted at longerwavelengths•  Herschel presents thefirst opportunity to studylarge samples of galaxies Dole et al. 2006selected near the peak
  • 4. Planck Herschel
  • 5. HerMES+PEPGOODS North / HDF NorthGOODS South CDFS ECDFSLockman wide & deepExtended Groth StripBootesXMM/VVDSSWIRE fields (EN1, EN2, ES1)Spitzer-FLSAKARI SEP Courtesy of S. Oliver
  • 6. The Herschel ATLAS•  The widest area extragalactic survey with Herschel (~ 570 sq deg)•  Consortium of 150+ astronomers worldwide led by Nottingham (Dunne) and Cardiff (Eales)•  Covering 5 bands with PACS and SPIRE (100 – 500 microns) in fast parallel mode•  5 sigma sensitivities of 132, 126, 33, 36 and 45 mJy / beam from 100-500µm•  Detect ~105 sources to z~3•  SDP = 3% of data = 7000 galaxies = 16 hrs!
  • 7. NGP & Equatorial Fields•  Chosen to maximize overlap with existing & planned survey data: GALEX, 2dF, SDSS, GAMA, UKIDSS, KIDS, VIKING, PanSTARRS, DES, MeerKAT, LOFAR , ASKAP etc SGP
  • 8. GAMA 9hr field(Driver et al. 2011)
  • 9. The Herschel ATLAS Pascale et al 2010•  250/350/500um•  no filtering•  cirrus background•  almost confused
  • 10. The dust SED z=0•  Sensitive to cold and warm dust giving the total mass of dust (and gas)•  At high redshift, the shape of the curve means that galaxies don’t get much fainter at larger distances.•  Study evolution of dusty star forming galaxies over the past 10 billion years of cosmic history•  The sub-mm colours of the galaxies will give us clues to their redshifts
  • 11. Cross-matching: the problem•  250um: –  beam 18.1” –  positional uncertainty ~2.4” –  minimal z info –  probes dust properties•  SDSS r band: –  PSF ~1-2” –  positional uncertainty ~0.1” –  redshift & colour information –  probes starlight/AGN Smith et al. 2011
  • 12. Identifying counterparts (Smith et al. 2011) •  Likelihood ratio technique (e.g. Sutherland & Saunders 1992) “The ratio of the probability that two f (r)q(m) sources are associated to the probability LR = that the same two sources are unrelated” n(m) 1 ⎛ −r 2 ⎞ Radial probability density – f (r) = exp⎜ ⎜ 2σ ⎟⎟ estimate from comparing 2πσ pos ⎝ pos ⎠ € HATLAS & SDSS positions n(m) = Probability density of possible counterparts i.e. SDSS r band number counts€ q(m) = Probability density of true counterparts – statistical excess€
  • 13. Identifying counterpartsIntroduce the Reliability: “The ratio of the probability that two sources are associated to the Li Rprobability that the same two sources i = ∑ ( are unrelated” Q0 L j + 1− ) Radial probability density – j estimate from comparingCan define a catalogue of 5sigma HATLAS & SDSS positions250um sources with R>0.8 opticalcounterparts.€ Smith et al. (2011)
  • 14. Identifying counterparts•  LR method allows for the fact that not all 250um galaxies are detected in Sloan r band:•  Q0 = ~63% of 250um sources have an r band counterpart in SDSS Smith et al. (2011)
  • 15. Identifying counterparts•  LR method allows for the fact that not all 250um galaxies are detected in Sloan r band:•  Q0 = ~63% of 250um sources have an r band counterpart in SDSS Smith et al. (2011)
  • 16. H-ATLAS: Complete SEDs •  Smith et al., submitted
  • 17. Comparisons with other models • Normalised to LFir • Binned according to matched luminosities • 1sigma uncertainty regions shown in grey hatchings • CE01 models too hot for 250um selected galaxiesChary & Elbaz (2001) vs Smith et al. 2011
  • 18. H-ATLAS: The luminosity function Dye et al. 2010
  • 19. H-ATLAS: Evolution of dust Dust mass varies by factor of 5 - not T High z SMGs @ z~2.5(Dunne 2003) T=25KDunne et al. 2011
  • 20. H-ATLAS: Environments of dusty galaxiesHerschel sources in and around galaxy clusters Coppin et al. 2011 Excess of far-infrared sources towards the centre of galaxy clusters in the local Universe
  • 21. H-ATLAS: Environments of dusty galaxies Herschel sources in and around galaxy clusters Burton, MJJ, et al. in prep. Find a tendency for far-IR bright galaxies to reside in less dense environments that a matched sample of non-far-IR galaxies Far-IR bright sources Optical sourcesSuggests that gas is strippedout of galaxies in denseenvironments, thus hinderingstar-formation activity
  • 22. H-ATLAS: lenses in the SDP field Negrello et al., 2010, Science
  • 23. H-ATLAS: lenses in the SDP field Negrello et al., 2010, Science Negrello et al. in prep.
  • 24. H-ATLAS: lenses in the SDP field Negrello et al., 2010, Science Negrello et al. in prep.
  • 25. H-ATLAS: lenses in the SDP field
  • 26. H-ATLAS: lenses in the SDP fieldLens subtraction @ F160W Flux @ 1.6 µm ~ 10 µJy CREDITS: Rosalind Hopwood
  • 27. H-ATLAS: lenses in the SDP field To extract the maximum amount of science from these lenses, accurate redshifts of both the lens and the lensed source are required. SALT is going to be the leading telescope to obtain accurate redshifts of the lenses in the southern hemisphere (PI Leeuw). Redshifts for the lensed sources requires mm-wavelength observations of redshift CO. ALMA and ATCA will do this in the southern hemisphere.
  • 28. H-ATLAS: High-z galaxiesIsolating high-dusty galaxies(Negrello et al. 2010) 2.5 < z < 5
  • 29. Lensing in HerMESIsolating high-dusty galaxies(Negrello et al. 2010) 2.5 < z < 5 Wang et al. 2011
  • 30. Lensing in HerMESEvidence for lensing inducedcross-correlations betweenbackground (high-z) far-IRsources and foreground (low-z)optical galaxies Wang et al. 2011
  • 31. H-ATLAS: Galaxy Clustering Maddox et al. 2010
  • 32. H-ATLAS: Galaxy Clustering van Kampen et al. submittedClustering as afunction of z bycombining H-ATLASwith GAMA
  • 33. HerMES: Fluctuation Analysis Amblard et al. 2011, Nature Brightness fluctuation analysis of two HerMES fields H-ATLAS fluctuation analysis to follow this year, over ~30 degree scale!
  • 34. H-ATLAS: AGN-star formationOne of the keyunknowns inastrophysics is how Density of galaxies /magnitudeactive galactic nucleiinfluence the formationand evolution ofgalaxies. Luminosity Benson et al. (2003)
  • 35. H-ATLAS: AGN-star formationOne of the key Supernovaeunknowns in 2 mechanismsastrophysics is how Density of galaxies /magnitude proposed to stopactive galactic nuclei gas cooling toinfluence the formation form starsand evolution ofgalaxies. Feedback is not Active Galaxies understood in models of galaxy formation. Luminosity Benson et al. 2003
  • 36. H-ATLAS: BAL QSOs and unificationCao Orjales, Stevens, MJJ et al., in prepLong standing issue as towhether BAL QSOs are anearly stage in QSO evolutionwhen the outflow terminates aperiod of star formation, or justa simple orientation effect
  • 37. H-ATLAS: BAL QSOs and unificationCao Orjales, Stevens, MJJ et al., in prepLong standing issue as towhether BAL QSOs are anearly stage in QSO evolutionwhen the outflow terminates aperiod of star formation, or justa simple orientation effect
  • 38. H-ATLAS: AGN-star formation•  Hardcastle, Virdee, MJJ, et al. 2010
  • 39. H-ATLAS: AGN-star formation•  Hardcastle, Virdee, MJJ, et al. 2010
  • 40. H-ATLAS: AGN-star formationWith the larger sample wesee a higher star-formation rate associatedwith more powerful radiogalaxies.In line with current viewsthat powerful AGN arefueled by the influx of coldgas via galaxy mergers,whereas lower powerradio sources are fueledby the hotter ICM Virdee, Hardcastle, MJJ, et al. in prep. Hardcastle, Ching, MJJ et al. in prep.
  • 41. H-ATLAS: AGN-star formationOne of the key unknownsis accurate redshifts athigh-z and opticalemission-lineclassification of AGN andstar-forming galaxiesSALT observations aregoing to address thisissue (PI MJJ) Virdee, Hardcastle, MJJ, et al. in prep. Hardcastle, Ching, MJJ et al. in prep.
  • 42. H-ATLAS: Far-IR—radio correlation•  The far-infrared—radio correlation is key to using future radio surveys to measure the star-formation history of the Universe•  FIRC looks to be very similar at low and high redshift•  Puzzling - as would expect evolution! Jarvis et al. 2010, MNRAS, 409, 92
  • 43. H-ATLAS: Far-IR—radio correlation•  The far-infrared—radio correlation is key to using future radio surveys to measure the star-formation history of the Universe•  FIRC looks to be very similar at low and high redshift•  Puzzling - as would expect evolution! Jarvis et al. 2010, MNRAS, 409, 92
  • 44. The new generation of radio surveys (a factor of ~10 shallower than LOFAR deep field data and 100 times shallower than MIGHTEE Tier 3) McAlpine & MJJ in prep. 10 arcmin
  • 45. The likelihood ratio on the new radio surveys Resolution does matter EVLA B-array in continuum radio surveys for X-matching. Key to almost all science! ASKAP-EMU WODAN MeerKAT will excel at this compared to ASKAP and APERTIF! Currently extending to fainter fluxes using COSMOS data.McAlpine, Smith, MJJ, Bonfield in prep.
  • 46. The likelihood ratio on the new radio surveys Depth of optical/nearIR EVLA B-array data also crucial! Again the MeerKAT- K=22.6 K=20 MIGHTEE deep fields ASKAP-EMU will have the best optical/ WODAN near-IR data available!McAlpine, Smith, MJJ, Bonfield in prep.
  • 47. The likelihood ratio on the new radio surveys Depth of optical/nearIR EVLA B-array data also crucial! Again the MeerKAT- K=22.6 K=20 MIGHTEE deep fields ASKAP-EMU will have the best optical/ WODAN near-IR data available! Redshifts are also important for science exploitation. SALT-MOS observationsMcAlpine, Smith, MJJ, Bonfield in prep. will provide these (PI McAlpine)
  • 48. Radio surveys with SKA precursors Constraints on the evolution of star-forming galaxies
  • 49. Radio surveys with SKA precursors Constraints on the evolution of AGN
  • 50. The link to cosmologyRaccanelli et al. (2011) present several predictions of the constraintsthat can be obtained on modified gravity and the cosmology using thenew generation of wide-area radio continuum surveys.
  • 51. The link to cosmologyCosmology with the radio continuum surveys requires information frommost of the science I have presented. The redshift distribution of radio sources is fundamental to many tests, such as ISW, lensing etc The new surveys will be dominated by star-forming galaxies and low luminosity AGN. We know the least about the redshift evolution of these objects! Herschel gives us information on the evolution of the SFGsWilman, MJJ et al. 2010Raccenelli et al. 2011 Nikhita & Kim both working on this
  • 52. The link to cosmologyCosmology with the radio continuum surveys requires information frommost of the science I have presented.The evolution of bias is also key.This is one of the most uncertainfactors in the predictionpresented in Raccanelli et al.(2011)Using GAMA+FIRST and SDSS-Stripe82+EVLA data we can pinthis down to z~0.7 (Lindsay, MJJ& Percival in prep) Wilman, Miller, MJJ et al. 2008 Raccanelli et al. 2011
  • 53. The link to cosmology Cosmology with the radio continuum surveys requires information from most of the science I have presented. The evolution of bias is also key. This is one of the most uncertain factors in the prediction presented in Raccanelli et al. (2011) Using GAMA+FIRST and SDSS- Stripe82+EVLA data we can pin this down to z~0.7 (Lindsay, MJJ & Percival in prep) Wilman, Miller, MJJ et al. 2008 Raccanelli et al. 2011But for SFGs and starbursts can use the measurements from Herschel surveys
  • 54. Summary•  Herschel is providing new and important insights into the evolutionof galaxies, from the star-formation history of the Universe, theevolution of dust, the influence of AGN activity etc.•  Over the next year or so, Herschel will also be working in pinningdown the shape of dark matter haloes through strong lensing,magnification bias over ~500 sq.deg and clustering of starburstgalaxies at z~2.•  We are using the techniques developed for Herschel and thescience results from Herschel to input into the design andimplementation of the new generation of radio continuum surveys.•  All of this information is key for our understanding of both galaxyevolution and cosmology