4 Comparison of the ALMA and Herschel - ESO

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data from ALMA, in addition to the contributions from Herschel, the size of databases and sophistication of models will increase dramatically. 44
7 Summary The PACS and SPIRE bolometer systems on Herschel are well suited to surveying large regions of the sky, whereas ALMA can provide high sensitivity, high angular resolution images in spectral line and continuum at longer wavelengths for regions of a few arc minutes in size. Thus, ALMA is better suited to be a follow-up instrument for Herschel surveys. Such follow-ups could be measurements of CO rotational transitions to determine the redshifts of sources detected in the dust continuum or broadband continuum to provide the component of Spectral Energy Distributions (SEDs). For spectral lines, ALMA will be complementary to Herschel because of different angular resolutions, frequency ranges and effect of the Earth’s atmosphere. For any spectral line surveys with Herschel, follow-up measurements with ALMA will greatly increase the scientific value, but it must be stressed that there should be an effort to make the Herschel surveys as complete as possible. ALMA images of many spectral lines will allow better estimates of source sizes. With Herschel one can measure line intensities for entire sources, but ALMA images would give estimates of the true source sizes, and thus the actual abundances of species, exactly those needed for chemistry models. Water vapour is a case of particular interest. High angular resolution images of the 183 GHz line of H 2 O and the 203 GHz line of H 2 18 O in ALMA Band 5 will be useful to supplement the lower angular resolution measurements of many lines of water vapour planned with Herschel HIFI. For protostars and molecular clouds the abundance of H 2 O will have an important influence on the energy balance and chemistry. In the study of protostars, the angular resolution of ALMA is needed to determine the sizes of components and variations of abundances on scales finer than a few arc seconds. Herschel would provide measurements of SEDs and line transitions that cannot be done with ALMA. Similar considerations apply to envelopes of AGB stars and Solar System objects. 45
Page 3 and 4: Report by the ESA-ESO Working Group
Page 5 and 6: Contents 1 Executive Summary ......
Page 9 and 10: 1 Executive Summary The Herschel Sa
Page 11 and 12: 2 Introduction The Herschel satelli
Page 13 and 14: 3 Descriptions of Herschel and ALMA
Page 15 and 16: Table 1: ALMA Antenna Arrays and Co
Page 17 and 18: 3.2 Herschel Herschel is a cornerst
Page 19: Table 6: Some Characteristics of th
Page 22 and 23: Figure 6: A three-dimensional plot
Page 24 and 25: Figure 8: A plot of the Herschel HI
Page 27 and 28: 5 Common Calibration of ALMA and He
Page 29 and 30: 6 Specific Examples of Synergies Be
Page 31 and 32: 6.3 High Redshift Objects During th
Page 33 and 34: eview) have also revealed a new cla
Page 35 and 36: In addition to emission lines from
Page 37 and 38: y interactions. Consider the nearby
Page 39 and 40: Figure 12: Data for IC10. The integ
Page 41 and 42: matter interacts with the powerful
Page 43 and 44: In DRSP contribution 2.1.2, Kinetic
Page 45 and 46: The Orion KL region is one of the n
Page 47 and 48: degrees. The GLIMPSE survey is bein
Page 49 and 50: An example is DRSP contribution 3.3
Page 51: Figure 18: A schematic of the analy
Page 56 and 57: The full ALMA will be in operation
Page 58 and 59: calibration files and to a pipeline
Page 60 and 61: SWAS — Submillimeter Wave Astrono
Page 62 and 63: Falgarone, E., Hily-Blant, P., Pine
Page 64: Wilson, C. D., 2005 in Proc. of The

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