Multi-wavelength surveys in the HerMES fields Nieves Castro-Rodríguez (IAC) Ismael Pérez-Fournon (IAC) Seb Oliver (Univ. Sussex) Antonio Cava (IAC) María del Carmen Argudo-Fernández (Univ. La Laguna) Cayetano Sánchez-Fabrés (IAC and Univ. Salamanca) Irene Pintos-Castro (Univ. La Laguna) Andrés del Pino Molina (Univ. La Laguna) Eduardo González-Solares (IoA, Univ. Cambridge) Evanthia Hatziminaoglou (ESO) and the SPIRE HerMES team

Herschel Space Observatory ESA cornerstone observatory (NASA;CSA and Poland) 3.5m Diameter Telescope, ~80K. The largest mirror ever built for a space telescope. Will perform Photometry and Spectroscopy in the FIR and submm region (60-670 μm). Two cameras/medium resolution spectrometers (PACS & SPIRE) + very high resolution heterodyne spectrometer (HIFI). To be launched in April 2009, minimum 3 years lifetime. • Study the formation of galaxies in the early universe and their subsequent evolution. • Investigate the creation of stars and their interaction with the interstellar medium. • Observe the chemical composition of the atmospheres and surfaces of comets, planets and satellites. • Examine the molecular chemistry of 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

The Herschel Multi-tiered Extragalactic Survey HerMES The 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 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 PACS: 160 micron and either 70 or 110 micron bands simultaneously (2 bands) SPIRE: 250, 350 and 500 micron bands simultaneously (3 bands) In SPIRE-PACS parallel mode: 70 or 110, 160, 250, 350 and 500 micron simultaneously (5 bands) Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

SEDs and Luminosities Herschel probes the rest-frame bolometric emission from galaxies as they formed most of their stars After Guiderdoni et al. MNRAS 295, 877, 1998 10 100 1,000 10,000 1000 1 0.1 1012L Z = 0.1 0.5 3 5 Flux density (mJy) l (mm) Herschel Herschel Peak around 200 microns (z=1) Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

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 Probed 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 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 Universe GTC … Best Survey fields Photometric Coverage X-ray -- XMM UV --- Galex Optical --- Various Mid-IR --- Spitzer Near-IR --- UKIDSS/VISTA Far-IR -- Herschel Sub-mm -- SCUBA-2/Apex Radio -- Various Redshift surveys… Magellan 100k redshifts AAT AAOmega ESO-VLT VIMOS Subaru FMOS Hectospec AGES GTC … Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

All the Aegis data of Groth Strip are available in this page 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 Madrid, December, 2008 Multi-wavelength Astronomy and the Virtual Observatory Workshop

ELAIS_N1 Lockman COSMOS 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 ELAIS_N1 Lockman COSMOS Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

Is there VO tools to locate the best data? A Multi-wavelenth Database: Is there VO tools to locate the best data? Deepest optical data Public data, etc … VO Center SPIRE Data Center Local (IAC) 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