Multi-wavelength surveys in the HerMES fields

1. 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

2. 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

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

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

5. HerMES The Herschel Multi-tiered Extragalactic 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 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 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

6. 0.5 Herschel 1 3 5 10,000 1012L Z = 0.1 1000 100 Herschel Flux density (mJy) 10 1 0.1 10 100 1,000 10,000 l(mm) After Guiderdoni et al. MNRAS 295, 877, 1998 SEDs and Luminosities Herschel probes the rest-frame bolometric emission from galaxies as they formed most of their stars Peak around 200 microns (z=1) Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

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

8. Fields, Areas and Depths: Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

9. 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

10. 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

11. Multi-wavelength data: Multi-wavelength Astronomy and the Virtual Observatory Workshop Madrid, December, 2008

12. Census of the Universe • 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

13. 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

14. 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

15. 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

16. 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