1. description of the proposed programme (max. 6 pages) 1...

1. Description of the proposed programme (max. 6 pages)

1.1 Scientific Goals:The primary aim of this proposal is to produce a data set crucial to a full and detailed understanding of keyphases in galaxy evolution. It specifically addresses questions concerning mass of the neutral interstellar medium(ISM), star formation rates, stellar dust return and interstellar dust properties. These are all closely related tothe large-scale process of galaxy chemical evolution. The Magellanic Clouds provide the unique opportunity tostudy such questions simultaneously galaxy-wide and in detail, as a function of both metallicity and radiativeenvironment (Fig. 1). Herschel SPIRE and PACS instruments are essential to provide key insights into thelife cycle of galaxies because the far-infrared (FIR) and submillimeter (submm) emission from dust grains is aneffective tracer of the coldest dust of the ISM, the most deeply embedded young stellar objects (YSOs), andthe dust ejected over the entire lifetime of massive stars.The ISM is imprinted by the astrophysical processes central to galaxy evolution. Mass, density, and temper-ature produce a range of ISM phases: cold molecular clouds, cold and warm neutral medium, warm and hotionized medium. The ISM gas cools from the warm to cold phases via atomic fine-structure line emission ina manner governed by metallicity. The formation of new stars consumes cold molecular gas. By their radiantenergy, the massive stars also convert this molecular phase into the warm neutral and ionized gas of photodis-sociation regions (PDRs) and HII regions. As the massive stars age, their winds blow bubbles and inject dustand chemically-enriched gas into the ISM. When they die, supernova blast waves inject tremendous energy intothe ISM mixing the nucleosynthetic products of stellar interiors with ambient gas. They disrupt and heat theISM while increasing its metallicity. This constant recycling and continuous enrichment drives the evolution ofa galaxy’s baryonic matter and changes its emission characteristics. Thus, to understand galaxy evolution, wemust study the physics of the ISM and its dynamic interaction with massive stars over entire galaxies.Why the Magellanic Clouds? The Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC)are the best astrophysical laboratories to study the lifecycle of the ISM, because their proximity (50 kpc, Feast1999; 61 kpc, Keller & Wood 2006) permits detailed studies of resolved ISM clouds and their relation to stellarpopulations on global scales, in an unambiguous manner, and as a controlled function of environment. In theMilky Way (MW), which is difficult to study in its entirety, all ISM studies suffer from confusion caused by line-of-sight crowding and distance ambiguity but in the LMC and the SMC, all features are at a similar distance,rendering masses and luminosities directly comparable. The thin-disk morphology and favorable viewing angleof the LMC in particular (35o, van der Marel & Cioni 2001) place only a single cloud along any line of sight.The LMC, SMC and Magellanic Bridge differ substantially in many global properties, which allows us to studyhow the processes governing galaxy evolution depend on these properties. The LMC has a Z∼ 0.25×Z� (Dufouret al. 1984), a mass of ∼ 8.7 × 109 M� (van der Marel et al. 2002), a size of ∼8 kpc (Kim et al. 1998) and acurrent star formation rate of 0.1 M� y−1 (Whitney et al. 2007). The SMC has a Z∼ 0.1×Z� (Dufour et al.1984), a mass of ∼ 2.4× 109 M�, a size of ∼3 kpc (Stanimirovic et al. 2004) and a current star formation rateof 0.05 M� y−1 (Wilke et al. 2003). The Magellanic Bridge is a filament of neutral hydrogen, which joins theSMC and LMC over some 15 kpc (Muller et al. 2004), is characterized by a lower metallicity than the mainSMC body (Z∼ 0.05×Z�) and has evidence of recent star formation adjacent to the SMC (Harris 2007).The metallicity of the LMC is similar to the metallicity of galaxies at the epoch of peak star formation in theUniverse (Madau et al. 1996; Pei et al. 1999). The metallicity of the SMC is similar to star forming galaxies atredshift ∼2 (Erb et al. 2006). In the LMC and SMC, dust-to-gas mass ratios are respectively ∼2 and ∼10 timeslower than in the MW according to UV extinction (Gordon et al. 2003); however, the infrared measurementsindicate lower values of ∼6 and ∼30 times (Bernard et al. 2007; Bot et al. 2004) which suggests that currentinfrared measurements are missing some of the dust. The lower dust content in both galaxies increases theambient UV radiation fields higher than in the Solar Neighborhood.The SMC and LMC have been surveyed at many wavelengths revealing structures on all scales thereby providinga rich context for our proposed study (Fig. 1). Historically, the Magellanic Clouds have played a key role inbridging the gap between the detailed study of astrophysical processes in the MW and the global study of theseprocesses in nearby galaxies. They have also been used as template galaxies for the more distant Universe. Interms of galaxy evolution, the LMC-SMC pair is uniquely suited to study how the agents of evolution, the ISMand stars, operate as a whole in two galaxies that are tidally interacting with each other and the MW (e.g.Zaritsky & Harris 2004; Bekki & Chiba 2005; Besla et al. 2007; Gardiner et al. 1996).Why the Herschel Observatory?We propose a uniform photometric survey (338 hrs) of the LMC (8 × 8.5 degrees), SMC and the Magellanicbridge (5 × 5 degrees; 4 × 3 degrees) in all SPIRE bands (250, 350, 500 µm) and the 100 and 160 µm PACSbands in order to produce a HERschel inventory of The Agents of Galaxy Evolution (HERITAGE), the ISMand massive stars. Full and uniform photometric coverage is necessary to understand these galaxies as completesystems, to understand the effects of metallicity, star formation rate, and stellar feedback on the ISM, to developtemplates for more distant galaxies, and to create an archival data set that promises a lasting legacy to matchcurrent LMC and SMC surveys at other wavelengths (Fig. 1).Herschel provides the crucial long-wavelength complement to our team’s Spitzer observatory studies of the LMC,SMC and Magellanic Bridge (Fig. 2). With the Spitzer IRAC and MIPS cameras, we have invested ∼> 1000

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1. Description of the proposed programme (cont.)

hours fully surveying the LMC and SMC over the full wavelength range (3.5-160 µm) and the IRS in targetedregions to study the lifecycle of galaxies (Fig. 1). These Spitzer studies were very successful in providinggalaxy-wide overviews of the emission of warm dust in the ISM, discovery of ∼>1000 YSOs, and a census ofthe mass injected by ∼>10,000 dusty evolved stars (Meixner et al 2006; Bolatto et al 2007). However, the totalinventory of the ISM is incomplete because Spitzer lacks the ability to trace the coldest components of the ISM,the earliest and coldest stages of star formation, the cold dust associated with evolved massive stars, and theinteraction of SNRs with the ISM (Fig. 2). Our analysis of the HERITAGE survey will provide a quantumleap in our knowledge of the ISM, current star formation, and evolved star mass-loss that will fundamentallyconstrain galaxy evolution theories (Figs. 1, 2, 3). In particular, we will address the following questions.Where is the mass located in the ISM? Submm emission from (cold) dust is an excellent tracer ofthe total mass of interstellar material, since the (Rayleigh-Jeans) emission is only moderately sensitive todust characteristics such as temperature and emissivity which affect the Spitzer estimates. The HERITAGEphotometric study with SPIRE and PACS directly measures the amount of (cold) dust on the scale of individualregions (∼ 10pc) in the LMC and SMC. At the distance of the Magellanic Clouds, we will detect (per beam,5σ) the emission from ∼ 0.1 M� of 25 K dust and ∼ 5 M� of 10 K at the shortest and longest wavelengths,respectively. This sensitivity corresponds to the equivalent of 0.85 × 1021 and 6 × 1021 H-atoms cm−2 forthe LMC and SMC (T=20 K dust, Fig. 2). This map of the dust mass over the LMC, SMC and bridge incombination with the existing HI (Kim et al. 2003, Stanimirovıc et al. 2000; Mueller et al. 2004) and CO maps(Fukui et al. 1999) will provide the dust-to-gas ratios for individual atomic and molecular clouds and, thus, anindependent check on the X-factor, the “constant” conversion factor between CO flux and H2 column density.Our analysis of this dust mass will elucidate the nature of the “very cold” emission observed in galaxies.Most estimates of the cold, dense-gas mass available for star formation rely on CO emission as a tracer for theH2 content of galaxies by assuming a constant X-factor that is locally ‘calibrated’ in the MW. However, at lowmetallicity molecular clouds may consist of thick surface layers of H2 and C+, “covering” small H2 and COcores and estimates of the molecular mass from the CO flux underestimate the total gas mass available for starformation (Israel et al., 1986, Poglitsch et al. 1995; Maloney & Black 1988; Pak et al. 1998; Roellig et al. 2006;Bolatto et al. 1999). Indeed, our Spitzer studies provide indirect evidence for cold hidden molecular gas inthe LMC and SMC through the presence of a FIR-excess emission component which is above and beyond thatexpected from HI and yet does not correlate with CO emission (Bernard et al. 2007; Leroy et al. 2007). Ouranalysis of HERITAGE data will reveal the dependence of the X-factor on environmental conditions such asmetallicity and local heating sources (Israel, 1997) that will have implications for the molecular mass estimatesfrom CO line fluxes in low metallicity galaxies at high redshift.Various lines of evidence indicate that the present accounting of the ISM of galaxies is incomplete, missing a verycold-dust-component and a substantial fraction of the molecular gas, particularly in regions of low metallicity(dwarf galaxies, outer parts of spirals, early universe). Recent studies have found ‘very cold’ dust emission(color temperature 4-7 K) in galaxies as varied as NGC 4631 (Dumke et al. 2004), NGC1569, a low-metallicitydwarf starburst galaxy (Galliano et al. 2003, Lisenfeld et al. 2002); blue compact dwarf galaxies in the VirgoCluster (Popescu et al. 2002) and the MW (Reach et al. 1995; Finkbeiner et al. 1999). The nature of the ‘verycold’ emission remains very uncertain. Suggested explanations include classical grains in shielded dense clouds(Galliano et al. 2003), fractal dust aggregates (e.g. Wright et al. 1993; Bernard et al. 1999; Stepnik et al. 2003;Lehtinen et al. 2004; Rawlings et al. 2005), the cold tail of a population of stochastically heated very smallgrains (Lisenfeld et al. 2002), and diffuse nonionizing UV radiation (Popescu et al. 2002). The difficulty ininterpreting the ‘very cold’ emission from Galactic studies lies in our inability to make absolute measurementsin the submm from within the MW. The difficulty in most extragalactic studies is the lack of spatial resolutionand hence wide range of temperatures within any given beam. HERITAGE will have the right combinationof submm sensitivity, resolution, and wavelength coverage, to map and measure the absolute brightness of thevery cold dust emission and thereby clarify its origin.What is the star formation rate in the Magellanic Clouds? The HERITAGE survey of the LMC, SMCand Magellanic Bridge will complete the census of star formation started with Spitzer. HERITAGE will be ableto detect the youngest and hence coldest objects – the starless prestellar cores and deeply embedded, cold class 0YSOs – in regions of star formation in the LMC and SMC. Herschel will be sensitive to YSOs more massive than4 M� in the Magellanic Clouds (Fig. 3). Moreover, the HERITAGE point source data will constrain the modelsof ∼>200 YSOs detected by Spitzer (Whitney et al. 2007) and thereby improve the estimates of such parametersas the total luminosity of YSOs, stellar mass, and total mass of dust (Robitaille et al. 2007). Approximately onequarter of the GMCS in the LMC have no active star formation based on Spitzer observations (Onishi et al., inprep) and the HERITAGE data will determine whether they contain class 0 sources or are truly starless GMCs.By completing the inventory of massive protostars and characterizing their environment, we can address keyscientific questions such as the total star formation rate and link this to the total local reservoir of cold materialdetected by Herschel (see above). In that way, we will quantify the star formation efficiency and determine thegas depletion timescale on a galaxy-wide scale, and determine the veracity of the Kennicutt-Schmidt law ona local scale. Comparison of LMC, SMC and Magellanic Bridge results with star formation in the MW will

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allow us to assess the importance of environmental parameters such as metallicity on these key aspects of starformation.What is the dust return by massive stars to the ISM? Massive stars could be important factories ofinterstellar dust either through their stellar winds or in the supernova ejecta. The significant dust observed inhigh redshift galaxies and quasars (Dwek, Galliano & Jones 2007 ; Bertoldi et al 2002) has been ascribed toinjection by massive stars, because low mass stars evolve too slowly. HERITAGE will complete the census of dustinjected into the ISM by massive evolved stars by measuring the colder dust associated with Red Supergiants(RSGs), Luminous Blue Variable (LBV), Wolf-Rayet (WR) stars and supernova remnants (SNRs) over a rangeof ages in the LMC/SMC (Fig. 3). Direct observations of newly formed dust in supernova ejecta in the MW arevery controversial differing by a factor 10 in some cases (Morgan et al 2003; Blair et al 2007) because studies ofdust in Galactic SN ejecta are confused along the line of sight with foreground or background material. In theLMC and SMC, the line of sight confusion is minimal and HERITAGE will be sensitive to dust masses ∼0.02M� of 25 K dust for a ∼10 pc diameter SNR in the LMC. By comparing the dust mass contributions of thedifferent massive evolved stars and SNRs, we can assess the relative importance of the stages and if the SNRstage destroys the dust produced by the evolved massive winds.What causes the variation in dust properties in the Magellanic Clouds? The variation in abundanceand properties of dust are of critical importance for understanding the thermodynamics of the gas, whenphotoelectric heating by PAHs and very small grains dominates. Ultraviolet studies have measured significantvariations in the extinction curve from sightline to sightline in the Magellanic Clouds (Gordon et al. 2003).Mid-infrared spectra show that the abundance of PAHs varies within the SMC from very low to nearly Galactic(Reach et al. 2000; Li & Draine 2002). In neutral diffuse regions of the LMC, the abundance of PAHs withrespect to total dust is similar to Galactic (Bernard et al. 2007) whereas PAHs are deficient in massive starformation regions such as 30 Doradus (Sakon et al. 2006). Herschel’s submm observations are crucial for thesemeasurements, since observations on the Rayleigh-Jeans portion of the spectrum are only mildly sensitive to thedust temperature, while the shorter-wavelength Spitzer observations are very sensitive to the temperature aswell as dominated (even out to 100 µm) by non-equilibrium emission from grains transiently heated by photonswith energy greater than the grain’s heat capacity (Fig. 2). HERITAGE, when combined with the Spitzerdata, will provide a complete map of dust properties in the Magellanic Clouds. Comparison of this map withtracers of the ISM gas phases and stellar populations will clarify how variations in dust properties correlatewith other processes in the Magellanic Clouds. Bernard et al. (2007) created a spatial map of 70 µm excessemission which reveals giant arcs near the 30 Doradus region, the most active massive star formation region inthe LMC, supporting the claim that this excess may be attributed to dust processing by massive star feedback,particularly, supernova blast waves. The shattering of dust grains has been theoretically predicted (Jones etal 1996; Tielens et al. 1994). The destruction of small grains behind the shock has been recently measuredin some LMC SNRs by Borkowski et al. (2006). On a galaxy-wide scale, the cumulative effect of supernovashocks theoretically controls the interstellar grain size distribution; and HERITAGE will be able to measuredust property variations quantitatively.

1.2 Exploitation Plan:The intensity of infrared emission from dust depends on the temperature and opacity/mass of the dust. We willderive dust temperature and opacity maps from the Herschel multi-wavelength images assuming an emissivity∝ να, with α = 2 initially and then determining whether variations in the emissivity index are required bystudying residuals. These maps can be used to understand trends in dust properties across the LMC and SMCISM (e.g. as in Bernard et al. 2007). Moreover, we will combine the Herschel SPIRE and PACS photometricbands with the Spitzer data at 3.6, 4.5, 5.6, 8.0, 24, 70, and 160 µm to completely constrain the SEDs of theindividual ISM dust regions for comparison with dust radiative transfer model calculations using models byDesert, Boulanger & Puget (1990), Galliano et al. (2003) or Gordon et al. (2001) (Fig. 2).For the YSOs, we will compare the measured SEDS from combined Herschel and Spitzer bands with theoreticalmodels of YSOs by Robitaille et al. (2007) and Whitney et al. (2004) to derive ranges for five physicalparameters: stellar mass, stellar temperature, stellar luminosity, envelope infall rate, disk mass. New modelswill be developed that include small clusters of YSOs in cloud cores. This will address both the issues of confusionat the LMC distance, and the contribution from the molecular cloud to the observed flux. The Herschel bandsprovide critical long wavelength constraints for the models; in particular the cold envelope characteristics. Forthe evolved massive stars, dusty RSGs, WRs and LBVs, we will fit dust radiative transfer codes such as 2Dust(Ueta & Meixner 2003) to estimate the dust mass-loss and total dust mass of these circumstellar shells intowhich supernovae will explode.1.3 Other Facilities: Herschel HERITAGE observations would fill a gaping hole in our understanding ofthe Magellanic Clouds; however, its interpretation will be done in the rich context of currently available surveys,many carried out by team members. The ISM gas which fuels star formation has been traced in HI 21 cm (e.g.Kim et al. 2003; Stanimirovic 2000) and CO (e.g. NANTEN, Fukui et al. 1999; Mizuno et al. 2001). Thestellar populations from which dust extinction can be derived have been measured in the optical (e.g. MCPS,Zaritsky et al. 2004) and near-IR (2MASS, SIRIUS, Kato et al. 2007). The warm dust emission has been

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observed extensively in over 1000 hours of Spitzer observations in programs such as SAGE (LMC;Meixner etal. 2006), S3MC (Bolatto et al. 2006), S4MC (PI: Bolatto), SAGE-SMC (PI: Gordon) and SAGE-Spec (PIs:Markwick-Kemper & Tielens), as well as the recent Akari satellite’s survey of the Magellanic Clouds. The SAGEteam has released a ∼>4 million point source catalog and final catalogs and processed images will be releasedin 2008. The S3MC catalogued 400,000 mid and far-IR sources, and SAGE-SMC is expected to increase thisnumber by an order of magnitude. In 2006, members of our team started conducting a survey of CI (609 µm)and higher rotational transitions of CO with the NANTEN2 telescope that will be very useful for interpretingthe PACS spectroscopy. We have recently submitted a LaBoca proposal to measure a number of regions at 870µm (PI: Hony). Members of our team are obtaining pointed observations of the Magellanic Clouds with Planck,that will provide even longer wavelength coverage. In the future, our Herschel program will provide essentialground work for future followup with Herschel, ALMA and JWST. We have no duplications with GTOs.

Fig 1: The HERITAGE survey of the Magellanic Clouds will use Herschel SPIRE 250, 350 and 500 µm andPACS 100 and 160 µm to map the mass of the ISM, particularly the cold dust component, with sufficientangular resolution (∼10 pc) to distinguish individual clouds. Top: The LMC showing the neutral atomic gastraced by HI (Kim et al. 2003) correlates well with the MIPS 160 µm (Bernard et al. 2007), the [CII] BICEmap shows [CII] emission outside of the molecular gas as traced by the NANTEN CO survey and the IRAC8 µm emission (SAGE; Meixner et al. 2006) is anti-correlated with the ionized gas traced by Hα (SHASSA,Gaustad et al. 2001). Bottom: The SMC and Magellanic Bridge at MIPS 160 µm (SAGE-SMC, PI: Gordon) isless well correlated with the HI (Stanimirovic et al. 2000). Right bottom: a blowup region showing the MIPS160 µm (SAGE-SMC + S3MC; Bolatto et al. 2007) emission detected by Spitzer and the anticipated PACS 160µm image which will have significantly better angular resolution. In fact, all of the Herschel SPIRE and PACSimages will have comparable (500µm) or better (all the rest) angular resolution than MIPS 160µm.

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Fig 2: SPIRE (250, 350 and 500 µm) and PACS (100 and 160 µm) on Herchel are the premier instruments tomeasure the presence of very cold dust missed by Spitzer and warm gas in the ISM of the LMC and SMC. TheSEDs of the entire LMC, based on data from Spitzer, IRAS and FIRAS (Bernard et al. 2007), and SMC, basedon data from Spitzer, IRAS (Leroy et al. 2007)and DIRBE (Stanimirovic et al. 2000). SEDS are fitted withthe dusty PDR model of Galliano et al. (2008, in prep). The Herschel SPIRE/PACS sensitivity corresponds tothe equivalent of 0.85× 1021 and 6× 1021 H-atoms cm−2 for the LMC and SMC, respectively, assuming 20 Kdust.

Fig. 3 Spitzer/MIPS/SAGE and predicted Herschel/HERITAGE fluxes vs. ratios of these fluxes for LMCsources (SMC sources will be ∼ 1.5× fainter). Templates based on SAGE MIPS 24, 70 and 160 µm datawith fluxes extrapolated to SPIRE/PACS bands using source models. HERITAGE will detect at least 2000point or compact sources based on the source extraction statistics of the SAGE MIPS bands. Its critical longwavelength will constrain at least 300 YSO Class I-II candidates, possibly clusters (blue circles) discovered inthe SAGE survey and modeled by Whitney et al. (2007). Moreover, it will be sensitive to ∼>4 M� Class 0 YSOscandidates (cyan circles), the templates of which are model predictions by Robitaille et al. (2006). HERITAGEwill detect all HII regions (pink squares) and constrain the dust mass of ∼>30 SNRs (red diamonds; templatesextrapolated from Spitzer measurements of Williams et al. 2006, 2007). Its long wavelength will constrain dustmasses from the massive evolved stars such as WR/LBVs (green triangles), and dusty RSGs (light brown circles;Srinivasan et al. in prep). Predicted point source sensitivity limits and confusion limits (which dominate andare estimated from the MC diffuse emission) for the Herschel/HERITAGE survey are a significant improvementover the SAGE limits in the overlapping bands.

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2. Technical Implementation (max. 3 pages)

2.1 Observations Strategy:

Fig. 4: The proposed HERITAGE PACS/SPIRE coverage is shown for the LMC (left) and SMC (right).Each rectangle shows the coverage of a single AOR over the SAGE MIPS 160 µm images (full SAGE-LMC andpreliminary, single epoch SAGE-SMC) and HI contours. The locations of the proposed PACS spectroscopicobservations are designated with white boxes. The lowest HI contour corresponds to a column density of8.5 × 1020 (LMC) and 1 × 1021 HI atoms cm−2 (SMC; see table and text). Only AORs for a single epoch areshown, the 2nd epoch AORs are very similar except rotated by 90o. This figure illustrates the HERITAGE goalof mapping the total (warm and cold) dust emission over the entire LMC & SMC.

Table 1 SPIRE and PACS Continuum MappingCharacteristic SPIRE Value PACS valuesurvey area 8◦× 8.5◦(LMC); 5◦× 5◦+ 4◦× 3◦(SMC)Total time (hrs) 212.5 (LMC), 125.5 (SMC)λ (µm) 250, 350, 500 100, 160angular resolution 18′′, 25′′, 36′′ 7.7′′, 12′′

physical scale for LMC (pc) 4.4, 6.1, 8.7 1.9, 2.9physical scale for SMC (pc) 5.4, 7.4, 10.6 2.3, 3.55σ at λ (mJy) 26, 36, 30.5 38.5, 555σ at λ (MJy/sr) 6, 4, 2 39.5, 18point sensitivity (LMC) ∼7 M� for T=10 K ∼0.35 M� for T=20 Kpoint sensitivity (SMC) ∼11 M� for T=10 K ∼0.53 M� for T=20 Kextended sensitivity (LMC) ∼ 9.2× 1021 H cm−2 for T=10 K ∼ 8.5× 1020 H cm−2 for T=20 Kextended sensitivity (SMC) ∼ 6.5× 1022 H cm−2 for T=10 K ∼ 6.0× 1021 H cm−2 for T=20 K

SPIRE and PACS Photometric Mapping in Parallel (238 hrs): For the full SPIRE/PACS imagingof the LMC & SMC, our science goals are primarily driven by the need to spatially map the cold (T < 15K) dust which requires SPIRE. The ability to acquire high quality PACS images at 100 and 160 µm for aminimum of extra time using the SPIRE/PACS Parallel mode fulfills the secondary science driver of gettingbetter wavelength coverage (100 µm) and spatial resolution (160 µm) of the large, warm (25 K < T < 15 K)grains. The LMC and SMC will be efficiently and fully mapped for the regions shown in Fig. 4 at 100, 160, 250,350, and 500 µm using SPIRE/PACS Parallel mode at low scanning speed (20”/sec). The low scanning speedmode was picked as it will allow us to reach our sensitivity goals as well as produce minimally smeared PACSPSFs. The AORs are designed to scan over each galaxy in long strips to ensure that background measurementsare made at the beginning and end of each scan leg which will allow for removal of the 1/f noise with timescaleslonger than the time to take a single scan leg. To further suppress the 1/f noise, each map will be repeated withthe scan angle rotated 90◦ which naturally happens in about 3 months at the positions of the LMC & SMC.Due to the large size of the LMC, we cannot obtain the 90◦ scan angle difference using the orthogonal mode asthis mode is limited to a width of 232′. Waiting 3 months to perform the 90◦ observations is necessary in orderto get the background measurements at the beginning and end of each scan leg.The map sizes for the LMC and SMC were chosen to fully encompass each galaxy as observed at 160 µm(Spitzer/MIPS) and in HI (see Fig. 4). In general, the proposed SPIRE/PACS observations are as large orlarger than the existing MIPS 160 µm observations as we found the MIPS 160 µm maps were slightly undersizedfor optimal background subtraction of the detected IR emission.

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2. Technical Implementation (cont.)

2.2 Observation Time Requirements:Our time request for SPIRE/PACS Parallel mode results in a high sensitivity to dust emission at a widerange of temperatures. The point source sensitivities translated to dust masses (assuming the standard 0.1 µmastronomical silicate dust grain) results in HERITAGE being able to detect dust emission at 5σ per beam inthe LMC of 0.1, 0.35, 1, 7, and 265 M� at temperatures of 25, 20, 15, 10, and 5 K, respectively. The SMCsensitivities are a factor of 1.5 higher (a larger distance). For extended sources, the sensitivities given in Table1 are translated to equivalent HI column density sensitivities using a gas-to-dust ratio 2x that of the MW forthe LMC. The corresponding sensitivities for the SMC are 7x higher (larger distance and a gas-to-dust ratio10x higher than the MW). We expect to smooth 6x6 resolution elements to achieve the a 5σ sensitivity of 1021

HI atoms cm2 which is necessary to detect the majority of the SMC bridge region.

2.3 Time Constraints: PACS spectroscopy has no timing constraints. The SPIRE/PACS Parallel imagingAORs include both sequence and timing constraints. The sequence constraints are required due to the need toefficiently map large regions using multiple AORs without introducing gaps between separate AORs. For theLMC & SMC, the scan angle rotates by 1◦/day. The timing constraints are used to most efficiently map theLMC & SMC given that they are not circular.

2.4 Robustness: In the event of a modestly decreased sensitivity in the SPIRE/PACS Parallel imagingmode would require us to smooth the observations to achieve our sensitivity requirements.

References:Bekki, K., & Chiba, M., 2005, MNRAS, 356, 680 Bennett, C.L.,et al., 1994, ApJ, 434, 587 Bernard, J.-P., et al, 2007, A & A, 347, 640 Bernard, J.-P., et al,2007, submitted to A & A Bertoldi, F, Cox,P, 2002, A & A, 384, L11 Besla et al. 2007, ApJ, 668, 949 Blair, W.P., et al., 2007, ApJ, 662, 998 Bock, J.J., et al.,1993, ApJ, 410, L115 Bolatto, A.D., et al, 2007, ApJ, 655, 212 Borkowski, K., et al, 2006, ApJ, 642, L141 Bot, C., et al., 2004, A & A, 423, 567 Dale, D.A.;Helou, G. 2002, ApJ, 576, 159 Dalgarno, A., McCray, R.A, 1972, ARAA, 10, 375 Desert, F.-X., et al, 1990, A & A, 237, 215 Dickman, R.L., et al, 1986, ApJ,309, 326 Draine, B.T., Bertoldi, F., 1996, ApJ, 468, 269 Dufour, R., et al, 1982, ApJ, 252, 461 Dumke, M., et al, 2004, A & A, 414, 475 Dwek, E., Galliano,F., & Jones, A. 2007, ApJ, 662, 927 Erb et al. 2006, ApJ, 644, 813 Feast, M., 1999, PASP, 111, 775 Finkbeiner, D.P., et al., 1999, ApJ, 524, 867 Fukui, Y.,et al, 1999, PASJ, 51, 751 Galliano, F., et al., 2003, A & A, 407, 159 Gardiner, L. T. & Noguchi, M. 1996, MNRAS, 278, 191 Gordon, K., et al., 2003, ApJ,594, 279 Gordon, K., et al., 2001, ApJ, 551, 269 Harris, J. 2007, ApJ, 658, 345 Heiles, C., 1994, ApJ, 436, 720 Hinz, et al, 2006, ApJ, 651, 874 Hollenbach,D, Tielens, A.G.G.M., 1997, RvMP, 71, 173 Hollenbach, D, McKee, 1989, ApJ, 342, 306 Isaak, K, et al, 2002, MNRAS, 348, 1035 Israel et al., 1986 ApJ 303,186 Israel, F., et al., 1996, ApJ, 475, 738 Israel, 1997 A&A 328, 471 Jones, A, et al, 1996, ApJ, 469, 740 Kato, D, et al., 2007, PASJ, 59, 615 Kaufman, M,et al, 2006, ApJ, 644, 283 Keller, S.C., & Wood, P. R. 2006, ApJ, 642, 834 Kim, S., et al., 1998, ApJ, 503, 674 Kim S., et al, 2003, ApJS, 148, 473 Lehtinen,K., et al., 2004, A & A, 423, 975 Lequeux, J., Allen, R. J., & Guilloteau, S. 1993, A & A, 280, L23 Li, A, Draine, B.T., 2002, ApJ, 576, 762 Madden, S., 2000,NewAR, 44, 249 Maiolino, R, et al., 2005, A & A, 440, L51 Maloney, P, Black, J, 1988, ApJ, 325, 389 Madau, P., et al, 1996, MNRAS, 283, 1388 Meixner,M, Tielens, AGGM, 1993, ApJ, 405, 216 Meixner, M. et al. 2006, AJ, 132, 2268 Mizuno et al. 2001, PASJ, 53, L45 Mochizuki, K., et al, 1994, ApJ, 430, L37Morgan, H.L., et al., 2003, ApJ, 597, L33 Muller, E. et al. 2003, MNRAS, 339, 105 Onishi, et al., 2007, in prep Pak, S., et al., 1998, ApJ, 498, 735 Pei, Y.C. et al. 1999, ApJ, 522, 604 Poglitsch, A., et al., 1995, ApJ,454, 293 Popescu, C.C., et al, 2002, ApJ, 567, 221 Popescu, C.C., et al, 2002, A & A, 361, 138Rawlings, M.G., et al., 2005, MNRAS, 356, 810 Robitaille, T, et al, 2007, ApJS, 169, 328 Roellig, M., et al., 2006, A & A, 451, 917 Reach, W.T., et al., 1995,ApJ, 451, 188 Reach, W.T., et al., 2000, A & A, 361, 895 Sakon, I., et al, 2006, ApJ, 651, 174 Stacey, G., et al, 1991, ApJ, 373, 423 Stanimirovic, S., et al,2000, MNRAS, 315, 791 Stanimirovic, S. et al. 2004, ApJ, 604, 176 Stepnik, B., et al, 2003, A & A, 398, 551 Tielens, A.G.G.M., 2005, Physics and Chemistryof the ISM, Cambridge University Press Ueta, Meixner, M, 2003, ApJ, 586, 1338 van der Marel, R., & Cioni, M.-R., 2001, AJ, 122, 1807 van der Marel, R.et al. 2002, AJ, 124, 2639 Whitney, B., et al., 2004, ApJ, 617, 1177 Whitney, B., et al., 2007, ApJ, in press Wilke, C.O., et al, 2003, A & A, 401, 873 Wolfire,M., et al. 2003, ApJ, 587, 278 Wright, E.L., 1991, ApJ, 375, 608 Zaritsky, D. & Harris, J. 2004, ApJ, 604, 167 Zaritsky, D., et al, 2004, AJ, 128, 1606

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3. Data Processing Plans (max. 2 pages)

3.1 Data Processing Plans:Processing Plan in state of revision.

3.2 Product generation justification:

3.3 Archival Value:

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4. Management and Outreach Plans (max. 2 pages)

4.1 Management Remarks: Management Plan is confidential to the team.

4.2 Outreach: Outreach plan will consist of a website

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5. List of Consortium Members

Margaret Meixner Space Telescope Science Institute, Full Astronomer/Webb Instrument Team Lead, PhD 1993 fromUC Berkeley Role: Principal Investigator of HERITAGE proposal. PI of the Spitzer SAGE survey of the LMC. 20 yearsexperience in ground-based, airborne and spaceborne IR astronomy; 68 refereed journal publications. PI of numerousprojects involving: circumstellar dust, dust radiative transfer, evolved stars, star formation, circumstellar molecular andatomic gas, photodissociation regions. 17 years experience in ground based IR instrumentation, PI of WHIRC camera,NIRIM camera. 20 year experience in millimeter interferometry. JWST/Mid-Infrared Instrument (MIRI) Science Team,Chair of National Herschel Science Center Users Panel. “Spitzer Survey of the Large Magellanic Cloud, Surveying theAgents of a Galaxy’s Evolution (SAGE) I: Overview and Initial Results,” Meixner, M.,; Gordon, K.; Indebetouw, R.; andSAGE Team 2006, AJ, 132, 2268; “Spitzer SAGE survey of the Large Magellanic Cloud II: Evolved Stars and InfraredColor Magnitude Diagrams,” Blum, R.D., and SAGE Team 2006, AJ, 132, 2034 “Models of Clumpy PhotodissociationRegions” Meixner, M. and Tielens, A.G.G.M., 1993, ApJ, 405, 216-228Suzanne Madden CEA Saclay, Service d’Astrophysique Role: science Co-I. PACS and SPIRE instrument team. Willadvise in data processing. 20 years experience in ground-based, airborne and spaceborne IR and submm observations.Expertise in the physics of the ISM of galaxies, especially gas and dust in low metallicity dwarf galaxies. co-PI of pointedPlanck Guaranteed Time proposal to map all of the SMC and LMC. “ ISM properties in low-metallicity environments”,Madden, S.C., Galliano, F., Jones, A.P. Sauvage, M. 2006, Astronomy & Astrophysics; “Tracing the [FeII]/[NeII] ratioand its relationship with other ISM indicators within dwarf galaxies” O’Halloran, B., Madden, S., Abel, N.P. 2007, A&A,submittedSacha Hony Service d’Astrophysique, Research Scientist SAGE project, PhD 2002 from University of AmsterdamRole: science Co-I and observation planning lead; Expert in IR spectroscopy with particular application to interstellarand circumstellar matter. “The CH out-of-plane bending modes of PAH molecules in astrophysical environments” Hony,S.; Van Kerckhoven, C.; Peeters, E.; Tielens, A. G. G. M.; Hudgins, D. M.; Allamandola, L. J. 2001, A& A, 370, 1030Alexander Tielens NASA Ames Research Center, Research Scientist/HIFI-Herschel project scientist, PhD 1982from University of Leiden Role: science Co-I, PDR and dust theory. 25 years experience in ground-based, airborne andspaceborne IR astronomy. 250+ refereed journal publications. PI of numerous projects involving PhotoDissociationRegions, interstellar Polycyclic Aromatic Hydrocarbon molecules, interstellar and circumstellar dust, gas and dust inregions of star formation, interstellar molecular and atomic gas “Physics and chemistry of the interstellar medium,”Tielens, A.G.G.M., 2005, University of Cambridge Press.Karl Gordon Space Telescope Science Institute, Assistant Astronomer, PhD 1997 from University of Toledo Role:PACS image processing lead, ISM dust and star formation. 10+ years of experience in interstellar dust related researchin the MW and nearby galaxies. 140+ refereed publications. PI of SAGE-SMC, the Spitzer Legacy Survey of the SmallMagellanic Cloud. member of the MIPS Instrument Team (8+ years). “The DIRTY Model. I. Monte Carlo RadiativeTransfer Through Dust” Gordon, K. D. et al. 2001, ApJ, 551, 269 “A Quantitative Comparison of SMC, LMC, andMW UV to NIR Extinction Curves” Gordon, K. D. et al. 2003, ApJ, 594, 279 “Reduction Algorithms for the MultibandImaging Photometer for Spitzer” Gordon, K. D. et al. 2005, PASP, 117, 503Alberto Bolatto University of Maryland, College Park, Assistant Professor, PhD 2001 Boston University, Role: PACSSpectroscopy lead, ISM gas research interest. 41 refereed publications. Over 10 years of experience in millimeter, submil-limeter, and far-infrared astronomy and instrumentation, not only as a user but also as an instrument builder (AST/RO;SPIFI, BIMA, CARMA). PI of the Spitzer Survey of the Small Magellanic Cloud (S3MC) and its spectroscopic follow up(S4MC). “The Spitzer Survey of the Small Magellanic Cloud: FIR Emission and Cold Gas in the SMC”, Adam K. Leroy,Alberto D. Bolatto, Snezana Stanimirovic, Norikazu Mizuno, Frank P. Israel, & Caroline Bot, 2007, The AstrophysicalJournal, 658, 1027 “The Spitzer Survey of the Small Magellanic Cloud: S3MC Imaging and Photometry in the Mid-and Far-Infrared Wavebands”, Alberto D. Bolatto, Joshua D. Simon, Snezana Stanimirovic, Jacco Th. van Loon, et al.2007, The Astrophysical Journal, 655, 212Charles Engelbracht University of Arizona, Assistant Astronomer PhD 1997, University of Arizona. Role: SPIREimage processing lead and science Co-I on ISM. The instrument scientist for MIPS and is the technical contact forthe SINGS and LVL Spitzer legacy programs. He supervised the postdoc (Bendo) and the data analyst (Block) whoperformed the SINGS, LVL, LMC (SAGE), SMC (SAGE-SMC) and MIPS guaranteed time data reductions. He is anexpert on MIPS calibration (Engelbracht et al. 2007) and in extended infrared emission from galaxies (Engelbracht etal. 2006).Ed Churchwell Albert E. Whitford Prof. Emeritus, University of Wisconsin-Madison; PhD, Indiana University 1970,Role: lead of source extraction group; PI of Spitzer GLIMPSE and GLIMPSE II projects; More than 35 years experiencein ground-based, airborne, and spaceborne IR astronomy and ground-based radio astronomy. Expertise in physics of theinterstellar medium and star formation, particularly HII regions, molecular clouds, and the interaction of newly formedstars with the ambient interstellar medium. “The Bubbling Galactic Disk,” Churchwell, E. et al. 2006, ApJ, 649, 759;“RCW49 at Mid-IR Wavelengths: A GLIMPSE from the Spitzer Space Telescope,” Churchwell, E. et al. 2004, ApJS,154, 322; “GLIMPSE: A SIRTF Legacy Project to Map the Inner Galaxy,” Benjamin, R. A., Churchwell, E. et al. 2003,PASP, 115, PASP, 115, 953-964Brian Babler Associate Researcher, University of Wisconsin; Role: develop point source extraction algorithms; over15 years experience processing space-based data; developed photometry routines for GLIMPSE IRAC pipeline.Tracy Beck Space Telescope Science Institute, Assistant Scientist, PhD 2001 from SUNY Stony Brook Role: PACSspectroscopy team, Integral Field Spectroscopy and IFU Reduction Specialist 9 years experience in ground-basedoptical/IR/mid-IR astronomy, 5 years experience as Near-Infrared integral field spectroscopic (NIFS) lead instrumentscientist; 19 refereed journal publications; JWST Instrument Team. Science interest formation of young massive starsand their feedback and impact on their environment. ”Investigating the Nature of Variable Class I and Flat-SpectrumProtostars Using 2-4 ?m Spectroscopy,” Beck, T. 2007, AJ, 133, 1673

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5. List of Consortium Members (cont.)

Jean-Philippe Bernard Centre d’Etude Spatiale du Rayonnement, Toulouse, France, Charge de recherches, PlanckScientist, PhD 1991 from Universite Paris XI Role: science Co-I 15 years experience in ground-based, balloon and space-borne FIR astronomy; 60+ refereed journal publications; PI of the PILOT balloon-borne experiment. Specializes intothe study of ISM dust properties, an observational cosmology. ”Spitzer Survey of the Large Magellanic Cloud, Surveyingthe Agents of a Galaxy’s Evolution (SAGE) IV: Dust properties in the Interstellar medium” Bernard J.P., Reach W.T.,Paradis D. et al 2007, submitted. ”Far-Infrared to millimeter astrophysical dust emission. I A model based on physicalproperties of amorphous solids”Meny C., Gromov V., Boudet N., Bernard J.-Ph., Paradis D., Nayral C. 2007, A&A 468,171Caroline Bot California Institute of Technology, Post-doc, Co-Investigator Role: analyze the spectral energy distri-bution of dust emission in the far infrared-millimeter. 3 year thesis on the interstellar medium and the dust cycle inthe Small Magellanic Cloud. 2 years of post-doc on the ISM conditions in nearby galaxies (inside the SINGS project)”Multi-Wavelength analysis of the dust emission in the SMall Magellanic Cloud” 2004, A&A 423, 567 ”Millimeter dustcontinuum emission unveiling the true mass of giant molecular clouds in the Small Magellanic Cloud”, 2007, A&A, 471,103Francois Boulanger Institut d’Astrophysique Spatiale, Research Scientist, PhD 1988 from University of Paris Pierreand Marie Curie Role: science Co-I. 25 years experience in infrared space missions IRAS, COBE, ISO and Spitzer.Herschel/HIFI co-I, member of the Planck consortium; 120 refereed journal publications; leader on numerous projects ondust, interstellar medium and star formation based on multiwavelength ground based and space observations and datamodeling; PI of the H2EX space mission proposed to ESA Cosmic Vision call. “Statistical properties of dust far-infraredemission, Miville Deschenes, M.A., Lagache, G., Boulanger, F., Puget, J.L. 2007, A& A 469, 595 “The first detection ofdust emission in a high velocity cloud, Miville Deschenes, M.A., Boulanger, F., Reach, W.T., Noriega-Crespo, A. , 2005ApJ 631, L57Steve Bracker retired, University of Wisconsin; Role: quality control on catalogs, diffuse source extraction; over 40years experience analyzing data in high-energy physics and infrared astronomy; performed quality control checks on theGLIMPSE and SAGE dataGeoffrey C. Clayton Louisiana State University, Professor, PhD 1983 from University of Toronto Role: Science Co-IISM dust. Over 25 years experience in ground- and space-based astrophysics; 116 refereed publications; PI of numerousprojects on HST, Spitzer, ISO, IUE as well as Gemini, VLT, and other large ground-based telescopes, studying circum-stellar and interstellar dust in Galactic, extragalactic, and the Magellanic Clouds “The Relationship Between Infrared,Optical, and Ultraviolet Extinction. Cardelli,” J.A., Clayton, G.C., and Mathis, J.S. 1989, Ap.J., 345, 245Martin Cohen Astronomer Step VIII, Univ. of California, Berkeley, USA. Role: ISM science; point source and diffusecalibration. 34 years of work on PNe; 17 years on absolute IR calibration; 242 papers in refereed journals, 32 on IRcalibration; “SPITZER SAGE Observations of Large Magellanic Cloud Planetary Nebulae”, J. L. Hora, M. Cohen &SAGE Team,2007, ApJ (revised)Kazuhito Dobashi Tokyo Gakugei University, Associate Professor, PhD 1994 from Nagoya University. Role: Compar-ison with extinction maps of LMC and SMC; 18 years experience in millimeter-submillimeter wave observations and darkclouds with extinction maps, 27 refereed journal publications “Atlas and Catalog of Dark Clouds Based on Digitized SkySurvey I”, K. Dobashi, H. Uehara, R. Kandori, T. Sakurai, M. Kaiden, T. Umemoto, S. Sato, 2005, PASJ, 57,S1-S386Yasuo Fukui Nagoya University, Professor, PhD 1979 from University of Tokyo Role: Star formation and ISM studiesStarted radio astronomy group and developed two 4m telescopes at Nagoya University. 162 refereed journal publications.Director of NANTEN sub-millimeter observatory situated in Chile. PI of numerous projects involving: star formation,Galactic structure, and Galactic center. Vice chair of ASAC in 2000-2001 and chair of ALMA commitee of NAOJ from1997 to 2005. Currently a member of EASAC.Frederic Galliano University of Maryland, Post Doc, PhD 2004 from University of Paris XI. Role: will participatein the analysis and modeling of the interstellar medium, especially the combined gas and dust diagnostics. Experi-ence: interstellar dust modeling and radiative transfer; photoionization, photodissociation; elemental and dust evolution,low-metallicity environments; stellar population synthesis. Select publications: (1) “Stellar Evolutionary Effects onthe Abundances of PAH and SN-Condensed Dust in Galaxies”, Galliano, F.; Dwek ,E.; Chanial, P. 2007, ApJ, ac-cepted, Astro-ph/0708.0790. (3) “ISM properties in low-metallicity environments. I. The spectral energy distribution ofNGC 1569”, Galliano, F.; Madden, S. C.; Jones, A. P.; Wilson, C. D.; Bernard, J.-P.; Le Peintre, F. 2003, A&A, 407,159-176.Jason Harris Associate Scientist, National Optical Astronomy Observatory, PhD 2000 from University of CaliforniaSanta Cruz Role: Science Co-I Research interests: star formation history of the Magellanic Clouds; physical processesgoverning star formation in galaxies; feedback to the interstellar medium from evolved stars (supernovae and asymptoticgiant branch stars).Joseph L. Hora Harvard-Smithsonian Center for Astrophysics, Astronomer/IRAC Project Scientist, PhD 1991 fromUniv. of Arizona. Role: Co-I interested in ISM and evolved objects/PNe. Experienced in ground- and space-basedIR instrumentation and astronomy; 66 refereed journal publications, 31 SPIE and technical papers; Project scientistfor Gemini NIRI camera, Spitzer/IRAC instrument; PI of Spitzer Legacy survey of the Cygnus-X region “The InfraredArray Camera (IRAC) For The Spitzer Space Telescope”, G.G. Fazio , J.L. Hora, et al. 2004, ApJS, 154, 10Annie Hughes PhD student at Centre for Astrophysics and Supercomputing, Swinburne University of Technology,Hawthorn VIC 3122, Australia. Thesis submission: 2008. Role: science co-Investigator Experience: PI of high-resolutionmapping survey of molecular gas in the LMC with the ATNF Mopra telescope. Local radio-FIR correlation in nearbygalaxies. Imaging techniques for wide-field radio continuum observations. “An ATCA 20cm Radio Continuum Studyof the Large Magellanic Cloud”, Hughes, A. et al. 2007, MNRAS, accepted. “Sub-Millimeter Observations of GiantMolecular Clouds in the Large Magellanic Cloud: Temperature and Density as Determined from J = 3-2 and J = 1-0Transitions of CO”, Minamidani, T. et al. 2007, ApJS, accepted. “A multiresolution analysis of the radio-FIR correlation

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in the Large Magellanic Cloud”, Hughes, A. et al. 2006, MNRAS, 370, 363.Remy Indebetouw University of Virginia and National Radio Astronomy Observatory, Research Scientist, previouslySpitzer Fellow. Experience with multiwavelength star formation studies in particular infrared through submm, as wellas infrared to radio data pipelines and software development. “The LMC’s Largest Molecular Cloud Complex: SpitzerAnalysis of Embedded Star Formation”, Indebetouw et al 2008 ApJ submitted “The protostellar population of the EagleNebula: Characterization using Spitzer/GLIMPSE”, Indebetouw et al 2007 in pressFrank Israel Full professor of Astronomy at Leiden University in the Netherlands (PH.D in Astronomy Leiden 1976).His main research interests are gas and dust in galaxy centers, and ISM and star formation in nearby galaxies, in partic-ular the Magellanic clouds. He is a recognised expert on the Magellanic Clouds and an experienced user of ground-basedfacilities (SEST, JCMT., IRAM, APEX) as well as airborne and space-based observatories (KAO, IRAS, Spitzer). Hewas one of the original proposers of FIRST, the precursor to Herschel. He has authored or co-authored over 200 papers,half of them in refereed journals.Akiko Kawamura Nagoya University, Post-doc, working for NANTEN and NANTEN2 radio telescopes. Role: starformation and ISM studies. Follow-up observations with submm ground based telescopes on MCs. “Giant molecularclouds in Local Group Galaxies,” Blitz, L, Fukui, Y., Kawamura, A., Leroy A., Mizuno, N., Rosolowsky, E., in Pro-tostars and planet V, 2007 “Detection of Molecular Clouds in the Magellanic Bridge: Candidate Star Formation Sitesin a Nearby Low-Metallicity System,” Mizuno, N., Muller, E., Maeda, H., Kawamura, A., Minamidani, T., Onishi, T.,Mizuno, A., and Fukui, Y. 2006, 643, L107Sungeun Kim Sejong University, Seoul, South Korea, Professor, PhD 1999 from the Australian National University.Role: Co-Investigator interested in the ISM and Star formation studies. Experience in radio, millimeter, submillime-ter, infrared, and optical observations and studies of the ISM/star formation in the LMC, Galaxy, and SubmillimeterGalaxies. “A Catalog of HI Clouds in the Large Magellanic Cloud” Kim, S. et al. 2007, ApJS, 171, 419. “CO J=4-3High-Velocity Cloud in the Large Magellanic Cloud” Kim, S. et al. 2005, AJ, 130, 1635. ”A Neutral Hydrogen Survey ofthe Large Magellanic Cloud: Aperture Synthesis and Multibeam Data Combined” Kim, S. et al. 2003, ApJS, 148, 473.Carsten Kramer (I. Physikalisches Institut, Universitaet zu Koeln, Germany), Assistant Professor. PhD 1992. Role:Life cycle of the ISM as it forms molecular clouds from the atomic phases, then forms stars which disperse the cloudsagain. Interested in particular in studying the contribution of [CII] from the different environments using models ofPDRs and of the ionized gas. Complementary observations with NANTEN2 and APEX. Co-I on the Herschel HEXGAL(galactic nuclei) and WADI (warm and dense Galactic ISM) guaranteed time key projects.Aigen Li Assistant Professor, University of Missouri-Columbia. Role: Science Co-I physics of interstellar dust, andthe infrared emission properties of galaxies. Li, A., & Draine, B.T. 2002, “Infrared Emission from Interstellar Dust. III.The Small Magellanic Cloud”, The Astrophysical Journal, vol. 576, pp. 762–772; Draine, B.T., & Li, A. 2007, “InfraredEmission from Interstellar Dust. IV. The Silicate-Graphite-PAH Model in the Post-Spitzer Era”, The AstrophysicalJournal, vol. 657, pp. 810–837Knox S. Long Space Telescope Science Instiute, Astronomer/Webb MIssion Scientist. PhD - California Instituteof Technology, 1976. Role: Co-Investigator. Science focus: Supernova Remnants and their interaction with the ISM.Experience: 30 years experience in studies of SNRs at UV, optical, X-ray and infrared wavelengths. More than 180refereed publications including initial X-ray survey of the Large Magellanic Cloud (Long, Helfand & Grabelsky 1979ApJ, 234, L77), optical identifications of SNRs in nearby Galaxies (Long, et al. 1990, ApJS 72, 61; Blair & Long, K. S.2004, ApJS, 155, 101) and Spitzer observations of Magellanic Cloud SNRs (Borkowski, et al. ApJ, 642, L141, Williamset al, ApJ, 652, L33)Massimo Marengo Harvard-Smithsonian CfA, Astrophysicist. Spitzer/IRAC GTO team. He is leading several Spitzerand HST GO and GTO projects in the field of mass loss from evolved stars, star formation and YSO jets, low mass starsand the study of young planetary systems/debris disks, with over 33 papers on refereed journals on these subjects.Ciska Markwick-Kemper Lecturer, Jodrell Bank Centre for Astrophysics, University of Manchester, PhD 2002from University of Amsterdam Role: science Co-I, PI of the Spitzer SAGE Spectroscopic Survey (SAGE-Spec) infraredand submm observations of dust and molecular gas, the astrophysics of dust, chemical composition, physical proper-ties, formation and evolution of dust grains “Dust in the Wind: Crystalline Silicates, Corundum, and Periclase in PG2112+059”, Markwick-Kemper, F. et al., 2007, ApJL 668, 107 “The Absence of Crystalline Silicates in the Diffuse In-terstellar Medium”, Kemper, F. et al. 2004, ApJ 609, 826Mikako Matsuura NAOJ/UCL, post-doc; scientific exploitation of evolved stars. Working on infrared astronomy ofevolved stars in our galaxy and galaxies in the Local Group. Extensive experience of the data analysis obtained withground (e.g. VLT, Subaru, JCMT) and space telescopes (e.g Spitzer, ISO). Modelling dust emission, molecular lines, aswell as atomic lines.Marilyn Meade Researcher, University of Wisconsin; Role: process data to produce point source catalogs; over 30years experience processing space-based data; processed over one million IRAC frames through the GLIMPSE pipeline.Karl Misselt University of Arizona, associate staff scientist PhD. 2000, Louisiana State University Role: science Co-I,and SPIRE team. Provides software and computer support for the SAGE and LVL Spitzer legacy programs. He is anexpert on MIPS calibration (Engelbracht et al. 2007; Gordon et al. 2007; Stansberry et al. 2007), extended emissionfrom cold dust in galaxies (Hinz et al. 2007), and modeling of emission from dust grains (Misselt et al. 2001).Erik Muller Australia Telescope National Facility, Bolton Fellow. Role: Co-Investigator researching the structure ofthe turbulent ISM in the MCs, as well as the relationships between the molecular and neutral ISM. PhD: 2004 fromUniversity of Wollongong, focusing on the neutral Hydrogen in the Magellanic Bridge. Current research focuses: themolecular component in the Magellanic Clouds, and it’s role in Star formation; ISM turbulence - the small-scale NeutralHydrogen of the SMC; Energy feedbacks and balance in the ISM. ”The origin of large-scale HI structures in the Magel-lanic Bridge” Muller, E., Bekki, K., 2007,MNRAS,381,11 ”Detection of carbon monoxide within the Magellanic Bridge”,Muller, E., Staveley-Smith, L., Zealey, W. J., 2003,MNRAS,338,609

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David Neufeld Professor of physics and astronomy at Johns Hopkins University. Role: science co-I, especially modelsupport of SNRs. His research interests are astrochemistry, interstellar medium, molecular astrophysics and infraredand submillimeter astronomy. He has experience both in theoretical modeling of astrophysical environments and inobservational studies that made use of the SWAS, ISO, HST, Spitzer, Arecibo and IRAM observatoriesAntonella Nota ESA HST Mission Manager at STScI, Head of Science Mission at STScI. Role: science co-I, massiveevolved stars and young clusters, experience with major ground based observatories (ESO NTT and VLT), and spaceobservatories (ISO, HST). 100+ papers in astronomical journals and conference proceedings. Carlson, L. et al. 2007,“Progressive Star Formation in the Young SMC Cluster NGC 602” ApJ 665L, 109 Nota, A. et al. 2006, “Discovery of aPopulation of Pre-Main-Sequence Stars in NGC 346 from Deep Hubble Space Telescope ACS Images ApJ 640L, 29Sally Oey University of Michigan, Department of Astronomy, Assistant Professor, Ph.D. 1995 from University ofArizona. Role: Co-Investigator, Science focus on how ISM and dust properties compare in regions of active feedback(SNR’s, superbubbles) vs in the diffuse ISM Experience: 15 years experience in multiwavelength studies of massive starsand feedback processes, including mechanical, radiative, and chemical feedback, as applied to galaxy evolution. Member,Board of Directors, International Gemini Observatory; 52 refereed publications. “A Reexamination of Observed andPredicted Stellar Ionizing Fluxes in the Large Magellanic Cloud,” Voges, E. S., Oey, M. S., Walterbos, R. A. M., &Wilkinson, T. M. 2007, AJ submittedKoryo Okumura Service d’Astrophysique of Commissariat a l’Energie Atomique, PhD in astrophysics 1993 from Uni-versite Paris XI, Role: PACS bolometer instrument specialist, PhD on the SMC with IRAS data, ISOCAM InstrumentDedicated team. Herschel PACS bolometer including the calibration through ground tests and the participation to thePACS science data simulator coding. The Herschel/PACS 2560 bolometers imaging camera, Billot, Nicolas; Agnese,Patrick; Augueres, Jean-Louis; Beguin, Alain; Bouere, Andre; Boulade, Olivier; Cara, Christophe; Cloue, Christelle;Doumayrou, Eric; Duband, Lionel; Horeau, Benoıt; le Mer, Isabelle; Lepennec, Jean; Martignac, Jerome; Okumura,Koryo; Reveret, Vincent; Sauvage, Marc; Simoens, Francois; Vigroux, Laurent, Space Telescopes and InstrumentationI: Optical, Infrared, and Millimeter. Edited by Mather, John C.; MacEwen, Howard A.; de Graauw, Mattheus W. M.Proceedings of the SPIE, Volume 6265, pp. 62650D (2006)Joana Oliveira Keele University, Postdoctoral Research Assistant, PhD Keele University, Postdoctoral Research As-sistant, PhD 2001, Role: Science Co-I: study of the physical and chemical properties of the early stages of star formation.Oliveira J.M., van Loon J.Th., Stanimirovi S., Zijlstra A.A., “Massive young stellar objects in the Large MagellanicCloud: water masers and ESO-VLT 3-4 um spectroscopy”, 2006, MNRAS, 372, 1509 van Loon J.Th., Oliveira J.M. etal., “ESO-VLT and Spitzer spectroscopy of IRAS05328-6827: a massive young stellar object in the Large MagellanicCloud”, 2005, MNRAS, 364, L71Toshikazu Onishi Nagoya University, Associate Professor, PhD 1996 from Nagoya University. Role: Star formationand molecular clouds; Follow-up observation on Magellanic Clouds in sub-millimeter wavelength with ground basedtelescopes. 16-year experience in millimeter-submillimeter wave observations and studies of low-mass star formation,55refereed journal publications. A Complete Search for Dense Cloud Cores in Taurus Onishi, T., Mizuno, A., Kawamura,A., Tachihara, K., & Fukui, Y. 2002, ApJ, 575, 950Deborah Paradis Ph.D October 2007, with Jean- Philippe Bernard at CESR in Toulouse, France. Post-doc next yearat the Science Space Center (Pasadena). Role: science co-I ISM dust. My scientific interest are the interstellar medium,dust emission (IR to millimeter), essentially studies of the variations of dust properties in the various phases of the ISM,combining data analysis and modelling.Albrecht Poglitsch MPE Garching, Senior Scientist and PI of PACS. 20 years experience in airborne and space-borne FIR instrumentation and astronomy; authored/coauthored 130+ publications; “A Multiwavelength Study of 30Doradus: The Interstellar Medium in a Low-Metallicity Galaxy”, Poglitsch, A., Krabbe, A., Madden, S. C., Nikola, T.,Geis, N., Johansson, L. E. B., Stacey, G. J., Sternberg, A., ApJ 454, 293 (1995). “The Photodetector Array Cameraand Spectrometer (PACS) for the Herschel Space Observatory”, Poglitsch, A., Waelkens, C., Bauer, O. H., Cepa, J.,Feuchtgruber, H., Henning, T., van Hoof, C., Kerschbaum, F., Lemke, D., Renotte, E., Rodriguez, L., Saraceno, P.,Vandenbussche, B., SPIE 6265, 62650B (2006).William T. Reach Caltech; IPAC Senior Research Scientist; PhD 1991 U.C.Berkeley Role: science and technical Co-ICurrently leading IPAC/Planck group to generate the Planck Early Release Source Catalog and US Planck data archive.Spitzer/IRAC instrument team leader 1999-2006. Performed absolute calibration of Spitzer/IRAC and COBE/DIRBE.Research interests include infrared emission from the ISM, diffuse clouds, supernova remnants. Over 100 refereed publi-cations. First-authored papers include: “A Spitzer Space Telescope Infrared Survey of Supernova Remnants in the InnerGalaxy”, 2006, AJ, 131, 1479 “Absolute Calibration of the Infrared Array Camera on the Spitzer Space Telescope”,2005, PASP, 117, 978 “Shockingly bright [OI] 63 µm lines from the supernova remnants W 44 and 3C 391”, 1996, A&A, 315, L277 “Atomic and molecular gas in interstellar cirrus clouds”, 1994, ApJ, 429, 672Thomas Robitaille Graduate student at the University of St Andrews, UK Role: science Co-I on YSOs. Developeda large grid of models SEDs for Young Stellar Objects which has been used to analyze point sources in Spitzer surveys,and will be used to analyze the combined Hershel and Spitzer data of the Magellanic clouds. “Interpreting SEDs fromYSOs. I. A grid of 200,000 YSO model SEDs”, T. P. Robitaille, B. A. Whitney, R. Indebetouw, K. Wood, P. DenzmoreApJS, 2006 (167, 256) “Interpreting SEDs from YSOs. II. Fitting observed SEDs using a large grid of pre-computedmodels”, T. P. Robitaille, B. A. Whitney, R. Indebetouw, K. Wood., ApJS, 2007 (169, 328)Douglas Rubin Service d’Astrophysique of Commissariat a l’Energie Atomique, student. Role: Science co-I, ISM.Expertise in FIR spectroscopy of the ISM. Currently using the SAGE data and [CII] data to study photoelectric heatingand [CII] emission from the ISM of the LMCMonica Rubio Full Professor, Departamento de Astronomia, Universidad de Chile Role: science Co-I 15 years ex-perience in ground-based mm and IR astronomy; 50+ refereed journal publications; PI of several projects involvingstudies of the interstellar medium, molecular gas and massive star formation in the Magellanic Clouds “Millimeter dust

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emission from an SMC cold molecular cloud”, Rubio, M., Boulanger, F., Rantakyro, F., Contursi, A. 2004, Astronomyand Astrophysics 425, L1.Marc Sauvage CEA/DSM/DAPNIA/Service d’Astrophysique, Saclay, France. PACS Co-I, SPIRE Asssociate Scien-tist, member of the PACS ICC. PhD in 1991 on the far infrared properties of the Magellanic Clouds and z=0 galaxies.Role: Science and technical co-I. Has extensive experience in space-based infrared astronomy (IRAS, ISOCAM, Spitzer).Principal science interests are: energy sources for the different dust phases of the ISM, infrared properties of metal-poorgalaxies, and embedded star formation in starburst galaxies. “ISOCAM mid-infrared spectroscopy and NIR photometryof the HII complex N4 in the Large Magellanic Cloud.” Contursi, A., M. Rubio, M. Sauvage, D. Cesarsky, R. Barba andF. Boulanger (2007). aap 469: 539-551. “The Spitzer view of low-metallicity star formation. I. Haro 3.” Hunt, L. K., T.X. Thuan, M. Sauvage and Y. I. Izotov (2006). apj 653: 222-239. “Stellar clusters in dwarf galaxies.” Vanzi, L. and M.Sauvage (2006). aap 448: 471-478.Marta Sewi lo: STScI, Post-doctoral Research Associate, Ph.D. 2006 from the University of Wisconsin-Madison,Role: science Co-I; general interest in the area of massive star formation; UC and compact H II regions in the LMCbased on the Spitzer/SAGE data, co-leading the extensive study of the YSOs population in the LMC discovered by theSAGE survey.Joshua Simon Caltech, Millikan Postdoctoral Fellow, PhD 2005 from UC Berkeley Role: science Co-I 2 years experi-ence with Spitzer observations of the SMC studying young stars and the ISM; further experience studying all aspects ofnearby galaxies, ranging from dark matter to chemical evolution. “The Spitzer Survey of the Small Magellanic Cloud:Discovery of Embedded Protostars in the H II region NGC 346” Simon, J. D., et al. 2007, ApJ, 669, 327Linda J. Smith Reader in Astronomy at University College London and ESA Astronomer at STScI. Role: : scienceco-I, massive evolved stars, ISM interactions and young clusters Scientific interests include massive evolved stars and theirinteractions with their environments, young massive clusters. PI on many space and ground-based proposals.Publishedover 100 papers in astronomical journals and conference proceedings. “Ejected nebulae as probes of the evolution of mas-sive stars in the Large Magellanic Cloud” Smith, L.J., Nota, A., Pasquali, A., Leitherer, C., Clampin, M. & Crowther,P.A., 1998. ApJ, 503, 278–296. “Realistic ionizing fluxes for young stellar populations from 0.05 to 2× Z�” Smith,L.J., Norris, R.P.F. & Crowther, P.A., 2002. MNRAS, 337, 1309–1328. “Quantitative spectroscopy of O stars at lowmetallicity. O dwarfs in NGC 346” Bouret, J.-C., Lanz, T., Hillier, D.J., Heap, S.R., Hubeny, I., Lennon, D.J., Smith,L.J. & Evans, C.J., 2003. ApJ, 595, 1182–1205.Sundar Srinivasan Graduate student at Johns Hopkins University, Baltimore, USA Role: science Co-I interested inmass loss and circumstellar dust emission from evolved stars. Working on radiative transfer modeling of LMC asymp-totic giant branch (AGB) stars in the SAGE database ”The mass-loss return from evolved stars to the LMC: empiricalrelations for excess emission at 8 and 24 µm, Srinivasan, S., Meixner, M., Vijh, U. et al. (in preparation)Snezana Stanimirovic University of Wisconsin Madison, Assistant Professor, PhD 2000 from University of WesternSydney Role: science Co-I 11 years of experience in IR/radio observations and studies of the diffuse ISM in the SMC andthe Galaxy; 30+ refereed journal publications. Co-I on the Spitzer Survey of the Small Magellanic Cloud. ”Spitzer SpaceTelescope detection of the young supernova remnant 1E 0102.2-7219”, Stanimirovic, S., Bolatto, Alberto D., Sandstrom,Karin, Leroy, Adam K., Simon, Joshua D., Gaensler, B. M., Shah, Ronak Y., Jackson, James M., 2005, ApJ, 632, L103“Cool Dust and Gas in the Small Magellanic Cloud”, Stanimirovic, S., Staveley-Smith, L., van der Hulst, J.M., Bontekoe,Tj.R., Kester, D.J.M., 2000, MNRAS, 315, 791Jacco van Loon Keele University, Lecturer/Leverhulme Research Fellow, PhD 1999. Role: science co-I, interested incold dust masses in evolved stars from PACS photometry. 12 years experience in IR/radio observations and studies ofmass loss from cool evolved stars. 69 refereed journal publications. “Dust-enshrouded giants in clusters in the MagellanicClouds”, van Loon J.Th., Marshall J.R., Zijlstra A.A., 2005, A&A 442, 597 “An empirical formula for the mass-loss ratesof dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars”, van Loon J.Th., Cioni M.-R.L.,Zijlstra A.A., Loup C., 2005, A&A 438, 273Barbara Whitney Senior Research Scientist, Space Science Institute; PhD 1989, University of Wisconsin; Role:Co-develop point source extraction pipeline and model YSOs. 106 refereed journal publications. Co-I on the SpitzerGLIMPSE and SAGE Legacy surveys; helped develop the GLIMPSE and SAGE IRAC processing pipelines; 25 yearsexperience in multidimensional radiation transfer. “Spitzer SAGE Survey of the Large Magellanic Cloud: III. Star For-mation and 1000 Newly Discovered Young Stellar Objects,” B. A. Whitney et al. 2007, AJ, submitted; “A GLIMPSEof Star Formation in the Giant H II Region RCW 49,” B. A. Whitney et al. 2004, ApJS, 154, 315-321; “2-DimensionalRadiative Transfer in Protostellar Envelopes: II. An Evolutionary Sequence,” B. A. Whitney, K. Wood, J. E. Bjorkman,& M. Cohen 2003, ApJ, 598, 1079-1099.M. Wolfire University of Maryland, Astronomy Department, Associate Research Scientist, Role: Co-I adds significanttheoretical expertise to the proposed investigation. A leader in modeling the chemistry, thermal structure and dynamicsof interstellar gas, particularly in the diffuse ISM, starforming regions and galaxies. “ [Si II], [Fe II], [C II], and H2Emission from Massive Star-forming Regions,” M. J. Kaufman, M. G. Wolfire, D. J. Hollenbach, ApJ, 644, 283 (2006)“Neutral Atomic Phases of the ISM in the Galaxy,” M. G. Wolfire, C. F. McKee, D. J. Hollenbach,& A. G. G. M. TielensApJ, 587, 278 (2003) “Far Infrared Submillimeter Emission from Galactic and Extragalactic Photo-Dissociation Regions:Models,” M. J. Kaufman, M. G. Wolfire, D. J. Hollenbach, & M. L. Luhman, ApJ, 527, 795 (1999) “The Neutral AtomicPhases of the ISM,” M. G. Wolfire, D. Hollenbach, C. F. McKee, A.G.G.M. Tielens, & E.L.O. Bakes, ApJ, 443, 152 (1995)

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6. Observations Summary List

AOT Time (hr) SSOs Timings Groupings Follow-up

SPParallel 338.0 6 22PSpecL 166.5

Notes (if applicable): AORs are grouped to ensure that the full survey area is covered by the separate strips.

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7. Alternative Observations Summary List

AOT Time (hr) SSOs Timings Groupings Follow-up

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1. description of the proposed programme (max. 6 pages) 1...

Documents