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 ( 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. 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

6. 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

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: 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 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

13. All the Aegis data of Groth Strip are available in this page
Public data of several waveleghts located in this web (
How many data are available using VO tools?
There are new data
Madrid, December, 2008
Multi-wavelength Astronomy and the Virtual Observatory Workshop

14. 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

15. 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

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 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