DDT Proposals

2012 DR 30, a strange object from the outskirts of the Solar System, has been discovered at the end of February 2012. Due to its special, high eccentricity and high inclination orbit it does not fit into any other object class identified so far and may be a first member of a new one. Herschel observations will detect the thermal emission from this body and with these fluxes we will be able to derive physical properties (size, albedo, etc.) of our target.

We propose to observe 2013 AZ 60, a newly discovered object on a highly eccentric orbit. Scan-map observations with the PACS photometer camera can unravel the main characteristics of the target including size, albedo and surface thermal properties. With these measurements we will be able to determine whether this object is an extinct comet or may rather be similar to 2012 DR30, a recently studied object an a similarly eccentric orbit that show surface properites more similar to that of main belt asteroids. As 2013 AZ60 has a likely origin in the Oort cloud but shows no cometary activity, with these measurements we have the rare opportunity to investigate an object from the least explored and furthest region of our Solar System. 2013 AZ60, as well as 2012 DR30, likely belong to a new class of large solar system objects (in the order of 100km in size) that could be potential sources or late representatives of the intrinsically brightest comets ever seen during human history.

Herschel observations of the large asteroid Ceres led to a major discovery, namely the first detection of an exosphere made of water vapour around an asteroid. The first detection occurred on 11 October, 2012, and was confirmed from HIFI observations conducted on 24th October and 6 March 2013 (guaranteed time program MACH 11, PI L. O'Rourke, and follow up from a DDT, PI M. Kueppers).

Observations of asteroids both for calibration and solar system science purposes have been an integral part of the Herschel mission right from the beginning. As the end of the mission is drawing nearer and nearer, an observation of the asteroid (2000) Herschel would be an appropriate 'last light observation', in addition providing valuable information allowing to determine the accurate size of this asteroid.

No abstract available

DDT: Shadow Observations of comet 67P Churyumov-Gerasimenko.

On May 25th this year, NASA announced the selection of OSIRIS-REx as part of its New Frontiers Programme. The OSIRIS-REx mission will be launched in September, 2016, fly by the Earth for a gravity assist in September, 2017, and encounter the carbonaceous asteroid 1999 RQ36 in November, 2019. Proximity operations at the asteroid last through March 2021, acquiring up to 60 g sample of its surface material. The Sample Return Capsule shall return to the Earth surface on September 25, 2023.

This proposal serves to obtain the first direct outgassing measurement of H2O from a confirmed to be active newly discovered Main Belt Comet using the HIFI instrument of Herschel.

Comet C/2012 S1 (ISON) was discovered in September 2012. Its orbit is nearly parabolic consistent with a dynamically new comet coming freshly from the Oort cloud. It is peculiar in that it is a sungrazer (q = 0.012AU) although not of the Kreutz group. This comet is expected to be the brightest comet for decades reaching a magnitude (according to Horizons) brighter than the full moon at closest approach to the sun. Journalists are calling it "the Comet of the century" and it is expected to have huge public outreach. This proposal serves to use the HIFI and PACS instruments to, in the former case, obtain the first detection of H2O from this comet, and in the latter case, derive a size estimate for the nucleus and determine its dust production rate. A total time of 5 hours (3 h HIFI, 2 h PACS) is being requested. HIFI is the most powerful instrument to detect water in distant comets, through observation of the fundamental water rotational transition which is much stronger than the transitions observable from the ground. The HIFI observations allows to detect H2O well outside the water dominated sublimation range (i.e. at heliocentric distances rh > 3 AU), a rare measurement for a comet. PACS is essential to detect the nucleus, its coma and any extended dust emission that may exist at that time. Our measurements will provide an important and unique reference for those wishing to track this comet for the remainder of the year. Unique in that the detection of early water outgassing from comet ISON can only be achieved with the Herschel Observatory because of its sensitivity and the spectral resolution o?ered by HIFI to e?ciently detect H2O. Observations of the H2O strong rotational lines cannot be performed from the ground. Unique in that we would be detecting the nucleus and dust cloud at 70 microns. These are unique measurements and unique solely to the Herschel Space Observatory and the European Space Agency; ideal for an ESA public outreach campaign.

The question of dwarf planet Ceres potentially being water rich is highly important for solar system science. A Herschel observation on 11 Oct. showed a clear detection of water absorption in Ceres spectrum, but only in H polarisation. An immediate reobservation is here requested.

On 16 September 2012 we got the first ever detection of the Ganymede water atmosphere with HIFI as part of the HssO GTKP, observing the leading side of this Galilean moon. The production processes of Ganymede’s atmosphere are debated. Possible candidates are sputtering/interaction with Jupiter’s magnetic field and sublimation. Since Jupiter’s magnetic field rotates faster than Ganymede’s orbital period, sputtering as the main production process should lead to a larger production rate at the trailing side of Ganymede. A more massive water atmosphere at the trailing side would therefore indicate that sputtering is the main atmosphere production process. If sublimation is the main production process the leading side atmosphere should be heavier, because the amount of ice exposed to solar irradiance is larger. We therefore propose an observation of Ganymede’s trailing side with 2 hours in Frequency Switch (FS) mode. We will also search for H2O gas in Callisto, targeting the first ever detection of Callisto's water atmosphere. We note that Callisto's surface has a lower albedo than either side of Ganymede, and a higher surface temperature. At the same time, the surface area of ice exposed to the Sun may be smaller than at Ganymede. Therefore, beyond the pure detection aspect, the measurement of Callisto's atmosphere will provide an additional element for the understanding the sources of the Galilean satellite tenuous atmospheres. Again, only 2 hours of HIFI time in FS mode are needed for the Callisto observation. There are three observation windows for Ganymede with the first starting on February 10 and one observation window for Callisto starting on 12 February 2013.

C/2013 A1 will make a close approach to Mars. Proposal to measure the size of the nucleus by taking images at 70, 100, and 160 microns to determine any hazard the coma or tail might have on the orbiting Mars probes.

We propose to observe the Apollo- and C-type asteroid 2005 YU55, which is on a Mars-Earth-Venus crossing orbit, during its upcoming exceptional Earth approach. In November 2011 it will pass within 0.85 lunar distances (0.85 LD) of the Earth, during which it will have a brief (less than one OD) observing window for Herschel. No asteroid of that size has ever been observed to pass inside 1 LD (and it will not happen again before 2028) although, according to recent orbit simulations, it does not pose any risk of an impact with Earth for the next 100 years. The proposed 0.3 hours of Herschel-PACS observations will allow us to characterize the object's size and its albedo. In combination with the foreseen radar measurements we will also be able to derive thermal surface properties which are strongly influencing non-gravitational forces, considered as one of the reasons for the large uncertainties in long-term orbit studies.

We propose to re-observe Apophis after opposition with very different surface temperatures to complete our thermophysical model study in terms of sense of rotation, thermal inertia and constraints on its interior.

We propose a 4-epoch PACS photometric monitoring, in coordination with Spitzer and ground-based telescopes, of the newly discovered young eruptive star V2492 Cyg, to verify our hypothesis on rapid re-arrangement of its circumstellar disk structure.

One of the key issues in astrochemistry is the identification of polycyclic aromatic hydrocarbons (PAHs). Herschel is a powerful tool to identify gas-phase interstellar PAHs, since these species have bands in the far-IR that are much more specific than the mid-IR ones. The Red Rectangle is the best object to search for these bands and we have obtained deep spectra with SPIRE and PACS. The PACS spectrum shows evidence of structures, which could be PAH bands. However, we were unfortunate to use high density sampling over short-range scans, and this results in "pointing noise" in the spectrum giving structures that are comparable to PAH features. We are asking for new PACS observations of the Red Rectangle using range spectroscopy with Nyquist sampling and 5 repetitions. Using this new data we will be able to reanalyze our high S/N data and determine which structures in the spectra are real astronomical signal and which are instrumental. With our optimized strategy, this observation requires 3.7 hours.

One of the key science goals of the HIFI instrument on Herschel has been the ability to quickly perform unbiased spectral line surveys. The hoped-for outcome, besides the analysis of known molecules through multiple lines, has been the detection of previously unknown species. And indeed, a number of unidentified lines have been found, both in emission and in absorption. The most spectacular, but also most puzzling of these is the 617 GHz absorption line feature first found toward Sgr~B2 and now seen in absorption towards other galactic sources. It is the only U-line found that does not trace the core or envelope of Sgr~B2, but rather the gas in the line-of-sight clouds in the spiral arms and Galactic center, between us and Sgr~B2. At present there is no known carrier for this feature. We request DDT observing time to improve a potential detection of this line in emission towards one galactic source and another source with narrow absorption lines. If the detection is confirmed the narrow lines of these sources will enable a search for hyperfine structure which can be used to narrow the search for molecular carriers.

Methanol emission peaks in cold gas, offset from protostellar activity, can be useful as signposts of recent ice mantle desorption. For the first time we detected water towards such a position and request DDT to maximize scientific value of the detection.

Methanol emission peaks in cold gas, offset from protostellar activity, are potentially useful as signposts of recent ice mantle desorption. We detected water towards such a position and request DDT to confirm theory by observing two additional sources.

We propose to observe a nearby candidate warm dust system, HIP 89046, that we have recently identified with WISE. Such debris disk systems are extremely rare, and therefore characterising each individual is extremely important to understand their origin and evolution. This object shows mid-IR emission from several instruments that is most likely associated with the star. There is also significant far-IR emission, which AKARI-FIS suggests is associated with a nearby object rather than HIP 89046, but may mask emission from HIP 89046 itself. There is therefore an ambiguity as to whether HIP 89046 is a protoplanetary disk, or a bona fide warm dust source. These observations will resolve this ambiguity, and possibly result in confirmation of a new record holder as the "dustiest" warm debris disk.

One of the early discoveries made with Herschel is the fascinating omnipresence of filamentary structures in all Galactic molecular clouds and the intimate relationship between these filaments and the star formation process. The physical origin of the dusty filaments imaged with Herschel remains an open issue, however. One likely possibility is that they originate from primordial structures in the diffuse, cold neutral (atomic) medium. We propose to use Herschel in parallel mode to image a unique region of the sky, centered on the Riegel-Crutcher clouds, where hair-like striations have been detected in HI absorption. These HI striations are aligned with the local magnetic field and parallel to faint dust filaments seen in Herschel Gould Belt Survey images of the adjacent Pipe molecular cloud. SPIRE has the sensitivity to detect the dust continuum emission from these faint HI striations (Av ~ 0.5), which will allow us to establish, for the first time, a direct connection between the filamentary texture of the cold atomic medium and that of star-forming molecular clouds.

Hi-GAL2pi will complete the 5-band far-IR survey of the Galactic Plane (GP), using PACS and SPIRE in pMode to map the two Galactic longitude areas that are not covered by the Hi-GAL KP nor its OT1 extension to the outer Galaxy. These two ~60° longitude-wide slices centered toward the cardinal directions l=90° and l=270° include critical regions with uniquely favourable observing conditions found nowhere else in the Galaxy: a) the longest available panoramic view of the Persus Arm, which is the arm with the least foreground contamination from the sun's viewpoint; b) the largely unexplored inter-arm region between the Persus and Carina Arms that spans most of the l=270° slice, that alone can be observed relatively free of confusion from our vantage point. The complete census of temperature, mass, and luminosity of filaments, clumps, cores and YSOs in these two regions will provide a spatially resolved measurement of the arm/inter-arm contrast in star formation rate (SFR) and efficiency (SFE), as well as a panoramic and unconfused view of the SFR and SFE along a full spiral arm extending from the Molecular Ring to the outer co-rotation Galactocentric radius. These observables, not accessible in the GP area covered in Hi-GAL KP or OT1 programs, will uniquely enable the critical steps in our understanding of the mechanisms responsible for the assembly, formation and fragmentation of the HI superclouds and the molecular clouds on spiral arms, and thus lay the foundations for a predictive global model of star formation in the Galaxy, that may serve as a template for Extragalactic studies. The completion of the Herschel Galactic Plane survey will establish a unique legacy that will be a keystone for all future Galactic and much extragalactic research, with data products that will be mined for decades by future generations and used for research not yet envisioned, with rich potential for serendipitous discoveries. Given our demonstrated community-oriented approach, we again waive our proprietary period.

Herschel\HIFI results suggest that hydrogen fluoride abundance is comparable to that of para-water over much of the interstellar medium, but not in the galactic center region where an enhancement of water abundance is observed. As part of the HEXOS GT KP, a strip scan of HF of a region of size 2" north and south towards the massive star-forming region of Sagittarius B2 (M) has been observed. We propose observations of a strip map of the para-H$_2$O fundamental line towards the same region. The H$_2$O strip would be extremely valuable to compare the spatial variations between HF and H$_2$O and will allow us to study the nature of the water abundance enhancement towards the galactic center.

An extraordinary variable protostar discovered during our SPITZER variability campaign shows significant brightness variation at PACS wavelengths. We request spectroscopy follow up to look for variation in CO, and [OI] lines to test the emission mechanism

An extraordinary variable protostar discovered during our SPITZER variability campaign shows significant periodic brightness variation at PACS wavelengths. Our effort to cover at least two maxima during our OT2 campaign failed due to severe straylight issues. That is why we request five epochs of photometer observation to cover the maximum of the lighturve of the source for the second time to confirm the amplitude changes that is expected based on the already obtained data.

The recent and unexpected detection of the most common fullerenes (C60 and C70) and proto-graphene in some Planetary Nebulae (PNe) raises the exciting possibility that other more complex fullerene-based molecules (e.g., carbon onions or multishell fullerenes, fullerene-adducts) might be ubiquitous in the Universe and continue to be serious candidates to explain many astrophysical phenomena. The presence of complex fullerene-based molecules such as carbon onions in the circumstellar shells of fullerene-containing PNe is strongly suggested by our recent analysis of the unusual diffuse interstellar bands detected towards two PNe where C60 had already been found. If complex fullerene-based molecules such as carbon onions are present in this peculiar class of stars, they could easily be detected in the far-IR range. Fullerene-containing PNe are usually very faint in the far-IR but our very recent detection of C60 fullerenes in PN IC 418 can now mitigate this unfortunate situation. Surprisingly, Herschel has not observed this very bright source - now considered the prototype fullerene-containing PN - as part of any approved program in previous cycles. Thus, a comprehensive far-IR study of the complex circumstellar environment where fullerenes and fullerene-based molecules may form is at present lacking. With this DDT proposal we aim at obtaining full range, high S/N, Herschel/PACS far-IR spectra of PN IC 418 to search for the spectral signatures of complex fullerene-based molecules such as multishell fullerenes (e.g., C60@C240, C240@C960), which are predicted to be detectable as relatively strong broad features in the far-IR range. If successful, these observations will constitute the first firm detection of the most complex molecules ever detected in space. In addition, we will search for the predicted hydrogenated amorphous carbon (HAC) associated feature at ~60 um to confirm/refute the HAC's processing/decomposition scenario as the preferred fullerene formation route in PNe.

We have found during our GT line survey of IRC+10216 and the search for hydrides (OT1 proposal) that some molecular lines present a strong intensity variation with time due to the role of infrared pumping. For some lines the intensity change in six months reaches a factor 3 (CCH). We have checked that the effect is not instrumental and than it arises from physical processes ignored so far in the radiative transfer models. We propose to observe the CCH and HNC lines within bands 1a-5b of HIFI every four months (three observing slots) to allow a detailed study of the variation of thermal molecular emission, and dust emission, in this prototype of AGB C-rich object. The settings will also provide, as a bonus, many lines of SiO, SiS, CS, HCN, CO and 13CO for which intensity variations of up to 30% have been found. In addition, a few specificc settings for HCN and CO will complete the observations. SPIRE and PACS observations will complement, with lower spectral resolution, the whole spectrum of each of these molecules and will provide a global view of the total intensity change of these lines with time. A crude estimate of the distance could be also obtained from the observed time lags between the blue and red parts of the line profiles observed with HIFI.

IRC+10216 is a Mira variable star with a long period of 649 days and an amplitude in K of 0.5 mag (Le Bertre 1982). Very recently, the first complete study with high spectral resolution of the submillimeter and farIR spectrum of this object has been carried out with HIFI (Cernicharo et al., 2010). In addition to the line survey of IRC+10216 a second program aiming at searching for light hydrides in this object was submitted and granted as GT1. The data of the line survey and those of the GT1 proposal were taken with 6 months of difference. We have been really surprised by the comparison of both set of data. Figure 1 shows some selected frequencies for which data is available from both proposals, while Figure 2 shows all CO, CS, and SiO lines that have been observed in both periods. Some lines show a quite remarkable variation in the intensity, in some cases by more than a factor of 2. The results are so surprising that we have checked all possible instrumental effects before giving credit to the new and unexpected physical processes involved in the emergent line profiles.

A subset of Asymptotic Giant Branch (AGB) stars loses mass at a very high rate. The dust effectively shields the radiation from the central star, allowing water-ice to condense onto existing silicate grains. Through the mass loss process, these stars provide a siginificant fraction to the gas and dust mass return to the interstellar medium. These so-called extreme OH/IR stars are thought to originate from stars with initial mass of 5 solar masses or more. These stars are expcted to experience the process of hot-bottom burning which preferentially synthesizes 13C and destroys 18O relative to the more abundant isotope. From HIFI observations of two of these objects, we observed a lack of H2_18O in these objects. Our aim here is to underpin the hypothesis of the high-mass progenitor of these stars by observing three isotopologues of H2O using HIFI in six other similar objects. Herschel offers the last opportunity to observe these lines for years to come.

Evolved stars are the birthplaces of the interstellar gas and solid dust particles. Such stars lose mass through a stellar wind, which is slow and dusty for cool giants and supergiants, or through impressive supernova explo- sions. However, recent observations with the PACS and SPIRE photometers reveal that the encounter between these slow and dusty winds and the interstellar medium is as spectacular as supernova explosions: multiple arcs, bar-like structures and different kind of instabilities (Rayleigh-Taylor and Kelvin-Helmholtz) are detected. The most outstanding example concerns the well-known supergiant Betelgeuse. However, with the current set of Herschel observations, it is impossible to define the exact physical mechanism causing the observed infrared emission. We propose to obtain PACS [O I] and HIFI [C II] spectroscopic observations at different pointings in the turbulent wind interaction zone around Betelgeuse. The proposed DDT observations would only take 3.1 hr and would give the astronomical community the first possibility to study spectroscopically the different dynam- ical and chemical processes partaking in the interaction zone between circumstellar and interstellar material. The derived spectroscopic information will be valuable to the whole community in preparation of OT2.

The phase-lag distance to the carbon star CW Leo.

This DDT proposal is the 'successor' to proposal DDT_mgroen01_6. In the original proposal we argued that it is possible to obtain a phase-lag distance to the well-known Carbon star CW Leo, and obtained 2 epochs of SPIRE time. In this proposal we present first results and demonstrate that the method works and present a first distance estimate. The dominant error is in the phase-lag, and we ask for 2 additional epochs to reduce this error, and obtain a more precise and accurate distance.

We propose to carry out imaging photometry of WISE J180956.27-330500.2 (hereafter WISE J1810) using PACS (at 70, 110, 160 micron) and SPIRE (at 250, 350, 500 micron) in order to obtain the latest far-IR and sub-mm fluxes of the object and constrain the nature of its mass-loss history. WISE J1810 was discovered very recently by us (Gandhi et al. 2012) as an object with a peculiar 2MASS--WISE spectral energy distribution (SED). We propose that the object is an asymptotic giant branch (AGB) star presently experiencing an episodic mass-loss event following a thermal pulse. If this is the case, it is the first opportunity of real-time observation of AGB mass ejection at thermal pulse. The infrared SED of this object is rapidly evolving over the past 15 years and updated observations over a broad wavelength range are essential. Herschel is the only available facility with the capability of high-sensitivity, high-spatial resolution observations at far-infrared and sub-mm wavelengths, and can provide indispensable information of the rapidly expanding dust shell of this object. The unique nature of this source, its recent bright appearance and rapid evolution prompt us to request a DDT observation while Herschel is still operating. The requested observing time is 1414 sec, which is the minimum operation time for the observing modes that will be used.

An exciting result of the first year of Herschel was the detection of massive molecular outflows (traced mainly by the OH molecule) in luminous dusty AGN, possibly providing the smoking gun of AGN feedback that is key to many models of galaxy evolution. All Herschel molecular outflow detections up to now are in luminous and distant systems (ULIRGs) or in nearby starbursts (NGC 253), while none of the nearbyt Seyferts observed so far showed clear outflow signatures, neither in Herschel spectra nor in ground based mm observations. Very recently, using IRAM PdBI, we have detected a massive molecular outflow in the nearby AGN NGC3079, via P-Cygni profiles of the HCN and HCO+ lines. By its proximity, this system could be a unique testbed for a spatially resolved Herschel study of such outflows, providing essential help in the interpretation of already ongoing GT and OT1 observations of more distant sources as well as stimulating and influencing further OT2 studies. Therefore, we suggest a DDT programme here, to observe several OH transitions of different energy level with PACS. The observations are tuned to deliver simultaneously, i.e. at no additional costs, lines of HCN, CO, and [CII]/

As part of the Herschel ULIRG Survey (HERUS) we have recently discovered within two objects extraordinarily powerful molecular outflows in OH. These outflows are substantially more powerful than those seen in Mrk231, which was the most powerful outflow source known to date. These two sources, IRAS 03158+4227 and IRAS 20100-4156, may thus host the two most powerful molecular outflows known in the Local Universe. The properties of these outflows have fundamental implications for understanding how AGN affect their environments. On a focused level, the AGN in these two sources are much more obscured than the AGN in Mrk231, implying that we may have caught these outflows in their earliest, most powerful phase. On a wider level, the impact of AGN outflows is thought to be critical in shaping the galaxy mass function at all redshifts, so the properties of these very powerful outflows in these two systems may be vital in understanding this impact. At the moment, however, we lack the data needed to constrain the properties of the outflows. We discovered the outflow signatures in the line profiles of the groundstate transitions of OH at 79 and 119 microns. From these two observations the total OH column density and covering factor of the outflow can be inferred, but not the all-important mass outflow rate and timescale. To do so, we need observations of the doublets of excited OH at 65 and 84 micron, since these excited levels are sensitive to the FIR radiation density around the source, and thus to the compactness of the outflow. Herschel is the only facility in the foreseeable future that can provide these data.

We request DD time to observe a highly magnified starburst at z=2.599 recently discovered with Planck, which has CO line widths like those of giant molecular clouds in the Milky Way! The velocity gradient and narrowness of the CO lines indicates that we are observing small (a few 10s pc) star forming regions in a distant galaxy due to its extreme magnification and fortuitous alignment with the lensing mass. This is a UNIQUE opportunity to probe a starburst at z=2.5 AT THE SCALE OF SINGLE STAR-FORMING REGIONS. We will measure [CII]158, the main coolant of UV-heated gas and thus, a prime tracer of star formation, and the H2 0-0 S(1) line, the main coolant of shocked gas, a tracer of turbulence dissipation and the warm molecular mass. Only Herschel can observe these important lines. ALMA cannot, and SOFIA cannot. During the formation process of galaxies, strong turbulence is generated with potentially dramatic consequences for the nature of star formation in distant galaxies. For example, if the gas remains turbulent on scales <100 pc, then the global galaxy kinematics (i.e., Toomre stability) no longer stabilizes the gas. What are the consequences for the star formation in such an environment and how does this high level of turbulence during galaxy formation change the nature of galaxies? Through a unique synergy of the Planck all-sky survey, Herschel, and IRAM sub-arcsec DDT interferometry, we have just caught a unique source at z=2.599, G80.3+49.8, with bright FIR continuum akin to dusty high-z starbursts, and surprisingly narrow CO line widths like GMCs in the Milky Way! G80.3+49.8 is truly unique and will become a benchmark for studying the physics regulating intense star formation at high-z. Herschel "last-minute" observations are our only way to quantify the global budgets of UV and shock heating estimated from the main IR cooling lines, both of which are unobservable from the ground, and both critical in linking the details of star formation with the generalities of galaxy formation.

We have recently discovered a z=2.50 heavily reddened (Av=6) hyperluminous K[Vega]=16.15) broad lined Type 1 quasar: ULAS J1234+0907 (Banerji et al, 2012, MNRAS in press) with a SMBH >10^10Msol (c.f. M87). This extremely rare type of lu...

With ALMA cycle 0 time we have observed 26 sources selected from the South Pole Telescope (SPT) survey, which covers 2500 deg^2 of sky area. These SPT sources are strongly lensed and the sample includes two of the most distant submm galaxies at z=5.7. The results of these observations reveal an unbiased redshift distribution of our sources peaking at z~ 3.5. We have started a follow-up started to observe the [CII] line in these sources. Combined with low-J CO lines we have already found tentative evidence for evolutionary effects in the ISM properties of our sources. We here propose to observe three SPT sources at 2

Using the PACS spectroscopic range mode, we propose to follow-up one of the most exciting discoveries of the Herschel mission: strong negative feedback in massive molecular outflows as traced by the OH molecule. Here we propose, for the first time in the far-Universe, to perform a sensitive observation in the ground-state OH 34 micron doublet in APM 08279+5255, a gravitationally lensed, radio quiet, broad absorption line (BAL) quasar at z=3.91. There is reason to believe that this source may be a scaled up version similar to local ULIRGs such as Mrk 231, with an apparent bolometric luminosity of L ~ 7 x 10^15 Lo: it is over three orders of magnitude more luminous than Mrk 231-, and with highly luminous radiatively pumped far-IR emission lines of H2O. The OH 34 micron line will be red-shifted to 170 microns in a sensitive PACS spectral region and will be observed in absorption against the extraordinarily strong rest-frame mid-IR continuum emission close to the peak of the quasar SED. It will provide the opportunity to study the extreme luminosity end of the feedback phenomenon in ULIRGs. By scaling the OH 34 micron absorption derived from our outflow models of the Herschel observations of Mrk 231 to the continuum level of APM 08279+5255, we estimate that 11.0 hours of observing time will be enough to detect the line with 5-sigma confidence; nevertheless, a stronger signal may be detected given the extraordinary properties of the source. If so, this will allow for velocity characterization of the flow. To our knowledge, this will be the first attempt to observe molecular outflows in hyper-ULIRGs in the early Universe and to test the current paradigm of negative feedback at the high end of the luminosity scale.

We propose a SPIRE FTS follow up of a newly discovered bright submm galaxy behind the Small Magellanic Cloud. The galaxy MMJ0107 was identified as a bright source at 1.1mm with AzTEC, with flux density of 43 mJy. There is no optical counterpart but the source is detected at radio (843 GHz), Spitzer/MIPS 24 µm, Spitzer/IRAC, WISE and NIR (J,H,Ks bands) as well as with Herschel SPIRE and PACS. The best photometric redshift estimate locates the galaxy at redshift ~2.8 and the SPIRE bands are bright enough (above 200 mJy at 350 µm) to allow spectroscopic follow up with the SPIRE Fourier-Transform Spectrometer. At this redshift, many of the ISM cooling lines will be within the FTS range: [CII] 157.7 µm, [OIII] 88µm, [NII] 122µm, etc. These considerations make MMJ0107 one of the best targets for FIR and submm spectroscopic follow up with Herschel and the photometric properties and the total IR luminosity give us confidence that we will detect lines in the FTS spectrum. This will increase the number of high redshift star-forming galaxies with positive line detections, which will further increase our knowledge of the physical conditions of these putative high redshift star-forming galaxies.

We have found an extremely bright (magnification of 20--60x; detected by 2MASS and WISE), extremely red lensed galaxy at z=0.82. Its WISE 22 um flux indicates SFR~1700 Msol/yr, but the morphology is a red spiral. We request 2.5 hr of DDT to obtain Herschel photometry with PACS and SPIRE.

We propose to obtain PACS/SPIRE imaging observations of XMM0044 at redshift z=1.58, one of the most massive, distant X-ray luminous cluster known to date, which was discovered within the XMM Distant Cluster Project. With the proposed data we will obtain an unbiased characterization of star-formation activity in the cluster galaxy population, at a critical epoch for cluster assembly. Based on its X-ray luminosity we estimate the cluster mass range to be [3.5-5]x10^14 Msun, indicating that this cluster already has a massive halo, at a cosmic epoch when cluster galaxies are observed to undergo significant structural and color transformation. Our optical NIR/IR follow-up observations unveiled a population of disturbed galaxies, with on-going star-formation and compelling evidence of merger activity in the brightest galaxies. The compact core with 4 galaxies within a radius of 3" is suggestive of the early formation stage of a BCG. The goal of this 10.2 hr program is to measure accurate star-formation rates of the cluster population in XMM0044 at z=1.6, by integrating the galaxies far-infrared (FIR) luminosity provided by PACS+SPIRE photometry. The observational window opened by Herschel straddles the critical peak of FIR emission of z=1-2 galaxies, providing a direct measurement of the on-going star-formation activity derived from the total infrared luminosity a technique that is unaffected by the uncertainties associated to extrapolations to the IR. Herschel is therefore fundamental to provide a view of the star-formation properties of distant galaxy clusters that up to now has been out of reach, in order to provide a comprehensive understanding of SF activity in high-density environments and the study of the evolution of the morphology-density relation. The requested observations will be the deepest FIR data of a high-z cluster, allowing us to reach star-formation rates as low as 50 Msun/yr (corresponding to Luminous Infrared Galaxies), a limit that is currently out of reach for z~1 clusters.

We proposed PACS photometry of SPT-CLJ2344-4242. It is the strongest cool core (CC) cluster known and is the only CC to be caught in a rare phase of the CC life-cycle when it is forming stars at a rate comparable to the inferred X-ray cooling rate.

Not available

We submit this DDT proposal to secure crucial SPIRE observations of a hitherto unexplored population of extremely mm-bright and radio-loud sources discovered by the South Pole Telescope (SPT). Only SPIRE observations can provide the adequate wavelength coverage (at 250, 350, and 500micron) to accurately constrain the spectral energy distributions of these radio-loud SPT sources, as well as their IR luminosities, dust temperatures, and redshift distribution.