Multi-wavelength surveys in the Multi-wavelength surveys in the HerMES fieldsHerMES fields

Nieves Castro-Rodríguez (IAC)Nieves Castro-Rodríguez (IAC)Ismael Pérez-Fournon (IAC)Ismael Pérez-Fournon (IAC)Seb Oliver (Univ. Sussex)Seb Oliver (Univ. Sussex)

Antonio Cava (IAC)Antonio Cava (IAC)María del Carmen Argudo-Fernández (Univ. La María del Carmen Argudo-Fernández (Univ. La

Laguna)Laguna)Cayetano Sánchez-Fabrés (IAC and Univ. Cayetano Sánchez-Fabrés (IAC and Univ.

Salamanca)Salamanca)Irene Pintos-Castro (Univ. La Laguna)Irene Pintos-Castro (Univ. La Laguna)

Andrés del Pino Molina (Univ. La Laguna)Andrés del Pino Molina (Univ. La Laguna)Eduardo González-Solares (IoA, Univ. Cambridge)Eduardo González-Solares (IoA, Univ. Cambridge)

Evanthia Hatziminaoglou (ESO)Evanthia Hatziminaoglou (ESO)and the SPIRE HerMES team and the SPIRE HerMES team

Herschel Space Observatory•ESA cornerstone observatory (NASA;CSA ESA cornerstone observatory (NASA;CSA and Poland)and Poland)•3.5m Diameter Telescope, ~80K. 3.5m Diameter Telescope, ~80K. The The largest mirror ever built for a space largest mirror ever built for a space telescope.telescope.•Will perform Photometry and Will perform Photometry and Spectroscopy in the FIR and submm Spectroscopy in the FIR and submm region (60-670 μm).region (60-670 μm).•Two cameras/medium resolution Two cameras/medium resolution spectrometers (PACS & SPIRE) + very high spectrometers (PACS & SPIRE) + very high resolution heterodyne spectrometer resolution heterodyne spectrometer (HIFI).(HIFI).•To be launched in April 2009, minimum 3 To be launched in April 2009, minimum 3 years lifetime.years lifetime.

••Study the formation of galaxies in Study the formation of galaxies in the early universe and their the early universe and their subsequent evolution.subsequent evolution.••Investigate the creation of stars Investigate the creation of stars and their interaction with the and their interaction with the interstellar medium.interstellar medium.••Observe the chemical composition Observe the chemical composition of the atmospheres and surfaces of of the atmospheres and surfaces of comets, planets and satellites.comets, planets and satellites.••Examine the molecular chemistry of Examine the molecular chemistry of the universe.the universe.Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

HerMESThe Herschel Multi-tiered Extragalactic Survey

HerMES is a 900hr = 3.2Ms, Guaranteed Time Key Project to study the evolution of galaxies at high redshift using ESA's Herschel Observatory. The survey is carried out by the SPIRE high-z Specialist Astronomy Group in Close coordination with the PACS Evolutionary Probe survey

PACS: 160 micron and either 70 or PACS: 160 micron and either 70 or 110 micron bands simultaneously (2 110 micron bands simultaneously (2 bands)bands)

SPIRE: 250, 350 and 500 micron SPIRE: 250, 350 and 500 micron bands simultaneously (3 bands)bands simultaneously (3 bands)

In SPIRE-PACS parallel mode: 70 or In SPIRE-PACS parallel mode: 70 or 110, 160, 250, 350 and 500 micron 110, 160, 250, 350 and 500 micron simultaneously (5 bands)simultaneously (5 bands)

Scientific Goals:Scientific Goals:

Provide a Legacy Study of the FIR Galaxy Populations.

Measure the Bolometric Luminosity Function of Galaxies At Redshifts z<3.

Characterise the Contribution of different Redshifts, Luminosities and Environments to the star formation.

Study the Galaxy Formation below the Herschel Confusion Limit

Combine all this with Surveys from other wavelengths to understand the Galaxy Formation and Evolution

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

SEDs and LuminositiesSEDs and Luminosities

Herschel probes the rest-frame bolometric emission from galaxies as they formed most of their stars

Herschel

After Guiderdoni et al. MNRAS 295, 877, 1998

10 100 1,000 10,000

10,000

1000

100

10

1

0.1

1012L

Z = 0.1

0.5

1

3

5

Flu

x d

ensi

ty

(mJy

)

(m)

Herschel

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

Peak around 200 microns (z=1)

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

Fields, Areas and Depths:

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

Redshift-Luminosity Space Redshift-Luminosity Space Probed by HerschelProbed by Herschel

This plot shows the redshift-luminosity space probed in a 4-tier wedding cake survey. Yellow: 0.25 square degrees, 1.7 mJy 5 threshold at 120 m (PACS); red, blue, and magenta: 0.9, 9, and 90 square degrees, with 5 thresholds of 10, 31, and 100 mJy at 250 m (SPIRE). The PACS and first SPIRE surveys would be confusion-limited.

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

Using Clusters as LensesUsing Clusters as Lenses

We will probe below the classical confusion limit with a number of techniques. One of these is to use the gravitational lensing of effect of galaxy clusters to separate and magnify background galaxies.

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

Multi-wavelength data:

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

Census of the Census of the UniverseUniverse

Best Survey fieldsBest Survey fieldsPhotometric CoveragePhotometric Coverage– X-ray -- XMMX-ray -- XMM– UV --- GalexUV --- Galex– Optical --- VariousOptical --- Various– Mid-IR --- SpitzerMid-IR --- Spitzer– Near-IR --- UKIDSS/VISTANear-IR --- UKIDSS/VISTA– Far-IR -- HerschelFar-IR -- Herschel– Sub-mm -- SCUBA-2/ApexSub-mm -- SCUBA-2/Apex– Radio -- VariousRadio -- Various

Redshift surveys…Redshift surveys…– Magellan 100k redshiftsMagellan 100k redshifts– AAT AAOmegaAAT AAOmega– ESO-VLT VIMOS ESO-VLT VIMOS – Subaru FMOSSubaru FMOS– Hectospec AGESHectospec AGES

– GTC …GTC …

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

All the Aegis data of Groth Strip are

available in this page

Multi-wavelength Astronomy and the Virtual Observatory WorkshopMadrid, December, 2008

•Public data of several waveleghts located in this web•(http://aegis.ucolick.org/astronomers.html)•How many data are available using VO tools?•There are new data

ELAIS_N1

COSMOS

Lockman

From Seb Oliver studies:

•xray--pink; •uv--cyan;•opt--green; •nir--brown; •mir--orange;•fir--red •submm--magenta (but scuba2 in red/black); •radio--yellow

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

Is there VO tools to locate the best data?Is there VO tools to locate the best data?– Deepest optical dataDeepest optical data– Public data, etc …Public data, etc …

VO CenterVO Center

SPIRE Data CenterSPIRE Data Center

Local (IAC)Local (IAC)

A Multi-wavelenth Database:

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

In short :•Herschel will be launched in April 2009

•Hermes will be an important survey to study the evolution of the galaxies at high z.

•We will have a large volume of data between 50-600 μm

•We will need complementary data in several wavelengths

•Only a small % are available using VO

•A local database always have addicional problems.

•We are thinking about solutions

Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008