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Report on the ALMA/Herschel Synergy
T. L. Wilson
European ALMA Project Scientist, ESO, Garching

ESA-ESO Meeting, Feb 10-11, 2005


Contributors (so far)
P. Andreani (Trieste) D. Bockelee-Morvan (Paris) J. Cernicharo (Madrid) P. Cox (Grenoble) C. De Breuck (ESO) D. Elbaz (Paris) E. van Dishoeck Leiden) M. Gerin (Paris) R. Fosbury (ECF-ESA/ESO) R. Laing (ESO) E. Lellouch (Paris) G. L. Pilbratt (ESA) P. Schilke (Bonn) C. Waelkens (Leuven) M. Zwaan (ESO)
ESA-ESO Meeting, Feb 10-11, 2005


Two major developments
Joint Herschel-ALMA meeting
Dusty04 in Paris October 2004; 200 participants Proceedings just published

FP6 ALMA enhancement proposal
Band 5 (160-210 GHz), contains H2O at 183 GHz, and H218O at 203 GHz for 6 to 8 antennas

ESA-ESO Meeting, Feb 10-11, 2005


ALMA Description
64 dishes with 12m diameter. These will be moved systematically from compact to extended configurations
Low-noise, wide-band heterodyne receivers whose outputs are connected to a digital correlator allowing high spectral resolution.

Will provide sensitive, precision imaging from 30 GHz (=1 cm) to 950 GHz (0.3 mm)
350 GHz (0.87 mm) continuum sensitivity: about 1 mJy in one second Angular resolution will reach ~0.05 arc seconds at 100 GHz (3 mm), and 10 km maximum separation of antennas The FOV for a single pointing ranges from 4' (at 30 GHz) to 10" (at 900 GHz)

ESA-ESO Meeting, Feb 10-11, 2005


ALMA Science Drivers
Key drivers:
High Fidelity Images in Spectral Lines and Continuum Measure dust broadband emission and spectral line radiation from atoms and molecules in high-z galaxies to obtain detailed morphology and kinematics: Protostars and planet formation:
Angular resolution of few AU at 150 pc (nearest molecular cloud)

ESA-ESO Meeting, Feb 10-11, 2005


Herschel: A 3.5 m telescope at L2
HIFI: Heterodyne single pixel system
480 to 1250 & 1410 to 1910 GHz FWHP beamsize 12" to 45"

SPIRE: Spectral and Photometric Imager
Bands at 250, 360 & 520 micrometers FWHP beamsizes 17", 24", & 35" Field-of -View (FOV) 4' by 8'

PACS: Photodetector Array Camera & Spectrometer
Bands at 60-85, 85-130 & 130-210 micrometers FWHP beamsize 7.7" (64 by 32 pixels) to 15.4" (32 by 16 pixels) FOV 1.75' by 3.5'
ESA-ESO Meeting, Feb 10-11, 2005


Science to be done with Herschel
HIFI: The study of the cycling of material from stars to the ISM SPIRE and PACS: To study how and when galaxies form To study the origin of planets, galaxies and the universe

ALMA wavelength range

ESA-ESO Meeting, Feb 10-11, 2005


Herschel and ALMA Science: The Cool Universe
Herschel is best suited for surveys, ALMA a followup instrument
ALMA has a small Field Of View (FOV), but high angular resolution and sensitivity Higher angular resolution to image the sources measured by Herschel Follow up to sources discovered with PACS or SPIRE in longer wavelength dust emission Also, surveys in CO to determine redshifts
ESA-ESO Meeting, Feb 10-11, 2005


Band 9 of ALMA plotted on Herschel HIFI Bands

There is some overlap in wavelength, but mostly the coverage of ALMA and Herschel-HIFI are complementary
ESA-ESO Meeting, Feb 10-11, 2005


The ALMA FOV is 25" at 1 mm

ESA-ESO Meeting, Feb 10-11, 2005


The ALMA FOV is 25" at 1 mm

ALMA Receiver Bands
ESA-ESO Meeting, Feb 10-11, 2005


Sensitivity with 6 antennas

Bands 3, 6, 7 and 9 are basic

ESA-ESO Meeting, Feb 10-11, 2005


Sizes of the SPIRE and PACS beam sizes on the HDF north Field
This shows the limits of Herschel angular resolution. Herschel measurements need follow ups with higher angular resolution imaging
ESA-ESO Meeting, Feb 10-11, 2005


UV

Visible

Infrared

mm

Add dust

Intensity

Wavelength
ESA-ESO Meeting, Feb 10-11, 2005


Scientific Areas
High Redshift Galaxies and Cosmology Active Galactic Nuclei & Star Formation in Galaxies Star and Planet Formation Water in the Universe Astrochemistry in Hot Cores and Envelopes of Evolved Stars Solar System

ESA-ESO Meeting, Feb 10-11, 2005


High Redshift Sources and AGN's
High star formation rates, >>20 solar masses per year Most of the radiation emitted by stars is absorbed by dust and re-radiated in the 3 micrometer to 1 mm wavelength range The luminous IR galaxies trace regions where the concentration of galaxies is largest, and trace the formation of large scale structures.

ESA-ESO Meeting, Feb 10-11, 2005


AGN's: Herschel & ALMA
Measure 1000's of sources with PACS and SPIRE, then follow up with longer wavelength continuum data with ALMA
spectral line measurements of CO and other species

Herschel will sample the regime where most of the luminosity is radiated
High resolution images with ALMA allow a better determination of the size of emission sources ALMA would provide high resolution images to refine models. Separate star formation and accretion in AGN's
ESA-ESO Meeting, Feb 10-11, 2005


Image of the redshift z=6.4 source in CO line emission
The CO emission was shown to be extended

ESA-ESO Meeting, Feb 10-11, 2005


Normalized integrated CO line intensity
With a number of CO line measurements one can determine physical parameters of a source

ESA-ESO Meeting, Feb 10-11, 2005


ESA-ESO Meeting, Feb 10-11, 2005


NGC6240-An AGN Case Study

NICMOS 1.6 micron

CO J=2-1 0.7" resolution IRAM Interferometer
2", 960 pc

ESA-ESO Meeting, Feb 10-11, 2005


Nearby Galaxies
Investigate star formation in other types of galaxies
At 10 Mpc, 0.1" is equivalent to 4.8 pc

Compare to models, in regard to the influence of nearby surroundings, metallicity, mergers

ESA-ESO Meeting, Feb 10-11, 2005


IC10-A Nearby Blue Dwarf Galaxy
D=0.7 Mpc; Total size of the image is 10'

ESA-ESO Meeting, Feb 10-11, 2005


Boxes show FOV of Bolometers. The FOV of ALMA at 3 mm is the circle in the lower left

Smallest box is the integral field spectrometer In PACS

ESA-ESO Meeting, Feb 10-11, 2005


Star Formation in our Galaxy
We can study different stages of star formation in individual sources We believe that the basic physical laws are understood but the relative importance of various effects is not known The study of low mass star formation will allow us to understand how our solar system formed In this study we group `protostars' and `debris disks'
ESA-ESO Meeting, Feb 10-11, 2005


Sketch of Protostar Development

ESA-ESO Meeting, Feb 10-11, 2005


450/850 micrometer images of Fomalhaut. The contours are 13 and 2 mJy/beam. Below are deconvolved images (data from JCMT and SCUBA)

ESA-ESO Meeting, Feb 10-11, 2005


Dust Spectra and Herschel Bolometer Bands

ESA-ESO Meeting, Feb 10-11, 2005


Orion KL Spectrum from Ground

ESA-ESO Meeting, Feb 10-11, 2005


Orion KL: The Classical Hot Core Source

Within a 20" region there are a variety of physical conditions
ESA-ESO Meeting, Feb 10-11, 2005


Red circles show the water Lines that can be measured with HIFI

This transition in ALMA Band 7

This transition in ALMA band 5 (a weak maser line and 18-O)
ESA-ESO Meeting, Feb 10-11, 2005


A Comparison of analysis schemes

ESA-ESO Meeting, Feb 10-11, 2005


Main Sequence & Evolved Stars
In broadband continuum, ALMA should be able to detect high mass stars in our Galaxy, and evolved stars even in the LMC In evolved stars such as IRC+10216, ALMA will be able to image molecular and dust emission
Herschel can be used to search for water vapor in the envelopes of such stars

ESA-ESO Meeting, Feb 10-11, 2005


Sample spectra from IRC+10216 (R Leo), a nearby carbon star

ESA-ESO Meeting, Feb 10-11, 2005


Images of some molecules in IRC10216, a nearby carbon star

ESA-ESO Meeting, Feb 10-11, 2005


Solar System Objects
Herschel can easily measure outer planets, and moons of these planets, as well as Trans Neptune Objects
Highly accurate photometry Water on the giant planets and comets Follow up would be HDO, to determine D/H ratio

ALMA and Herschel might be used to measure a common source at a common wavelength to set up a system of amplitude calibrators
ALMA provides high resolution image, but also records the total flux density
ESA-ESO Meeting, Feb 10-11, 2005


Recommendations for Future Work
Overall, Herschel is best suited for surveys, while ALMA a follow up instrument
ALMA has a small FOV, but high angular resolution and sensitivity Higher angular resolution to image the sources measured or detected by Herschel Also follow ups to PACS or SPIRE surveys in CO or in longer wavelength dust emission Complementary line surveys with HIFI and ALMA

In combining results we need well established calibrations In analyzing the results, need a much more sophisticated system
This is a part of the EU FP6 program `The Molecular Universe' and the science support within the ALMA European Regional Center

Bring the two communities together for the development of a far IR interferometer in space
ESA-ESO Meeting, Feb 10-11, 2005