Report on the 91 st ESO OPC Meeting. What Matters in an ESO Proposal

Report on the 91 st ESO OPC Meeting What Matters in an ESO Proposal Rainer Schoedel, IAA-CSIC Weekly Scientific Seminar of the IAA, 13.12.2012

General Information

Video streams ESO@50 available on ESO websites. 2013: HAWK-I will be removed when MUSE arrives (probably in P91). It will come back once the AOF is available on UT4 (~2015). NACO may be decommissioned soon (after next GC season, Aug 2013). ISAAC will be dismounted in June 2013. Parsec --> Perla (15W) GRAVITY: ~ 2014 Finances: Overall annual budget 130 M /yr base budget (fluctuating). 50 M must be saved over next decade. Brasil needed for E-ELT (+ Spain or France) Problems with exchange rates (swiss frank, Chilean peso); No (or very late) contribution from Spain this year: ESO had to take credits to be able to pay salaries but will not ask for the interest.

La Silla 2.2m not available after P91 3.6m and NTT max 50% of time as of 2016 (P97) VIMOS public surveys? Maybe future call for VIMOS spectroscopic surveys VIMOS so far used in narrow RA ranges (COSMOS field etc.) IF instrument successfully upgraded and observing backlog cleared, then Call for Letters of intent February 2013 with deadline 15 April 2013. VISIR will not be available for operations for the rest of P90 (to end March 2013). Affected PIs have already been contacted. Status for P91 unclear.

Breaking news 1. PERIOD 91 DELTA-CALL FOR ISAAC PROPOSALS On account of the technical problems encountered during the re-commissioning of VISIR (see announcement), about 400 hours of observing time have become available at UT3. For this reason, ESO invites proposals for observations at UT3 with the ISAAC near-infrared imager and spectrograph during Period 91. Owing to operational constraints and ongoing time commitments, requests are restricted to the RA range 12 to 22 hours. Although Service Mode is encouraged, the Observatory will consider and evaluate Visitor Mode requests based on their scientific requirements. Preference is given to programmes with loose moon constraints. However a fraction of the observations can be accommodated during dark time depending on the scientific justification. Proposals must be submitted using the P90 DDT template, which is available via the ESO User Portal. To allow for quick processing of the proposals, the Special Remarks section should contain the following statement: "ISAAC Delta-Call". In the case of a Visitor Mode request, a detailed justification should be given in Box 8b (DDT Justification). Proposals can be submitted any time before 20 January 2013. Applicants will be informed about the outcome of the selection process as soon as possible after the deadline. ESO Electronic Newsletter, Dec. 2012

Upcoming instruments

Upcoming instruments MUSE - in 2013

Upcoming instruments

Upcoming instruments KMOS - commissioning ongoing

Evaluation Procedure

Step by step Conflicts of the referees will be identified (and must be declared): e.g. institution, authorship, collaborations. Referees will not evaluate proposals when there exists a conflict. Pre-evaluation by the referees and triage process: lowest 30% of proposals will be rejected and not discussed (but may be resurrected). GTO and Chilean time will not be triaged. Discussion, final evaluation, feedback (by primary referees)

Evaluation Criteria

Evaluation Criteria Be especially careful with re-submissions.

Grades

Grades In order to be securely scheduled, a proposal should be above this line (and not require too specific conditions).

Grades In order to be securely scheduled, a proposal should be above this line (and not require too specific conditions). Any proposal below 3.0 will not be observed.

Backup mode There is no backup queue at the VLT. However, it is possible to obtain data as long as the proposal has not been triaged in pre-opc evaluation and has reached at least category C (3.0 or higher) in the final grades. Example: PI Schoedel, P89

Backup mode There is no backup queue at the VLT. However, it is possible to obtain data as long as the proposal has not been triaged in pre-opc evaluation and has reached at least category C (3.0 or higher) in the final grades. Example: PI Schoedel, P89 rejected

Backup mode There is no backup queue at the VLT. However, it is possible to obtain data as long as the proposal has not been triaged in pre-opc evaluation and has reached at least category C (3.0 or higher) in the final grades. Example: PI Schoedel, P89 grade C, but fully executed rejected

Backup mode There is no backup queue at the VLT. However, it is possible to obtain data as long as the proposal has not been triaged in pre-opc evaluation and has reached at least category C (3.0 or higher) in the final grades. Example: PI Schoedel, P89 grade C, but fully executed rejected Think carefully about required observing conditions! (other details matter as well: e.g., R.A. range)

Keep in Mind Each referee has to read 70-100 proposals (including ~10 large proposals). Typically 20-30 min of reading time for normal proposal (40-60 min for large proposal). Most proposals will only be read once. There will probably be an expert in your field in the panel, but many referees may not be familiar with your field or techniques: explain the relevant background and techniques. The referee must get a clear idea about what you are trying to achieve, how you will do this, and why this is of importance for astronomy in general.

Some Specific Points Know your instrument. Concrete goals. Be very specific about what you are trying to achieve. Clarity in text, and figures. Be clear on sample selection, sample sizes, linear and angular resolutions expected for your target. Take feedback serious. Important for re-submissions. Why would astronomers from other fields care about your observations, what is the larger context? If you observe an individual target, make clear what we will learn for the broader picture. Try to be quantitative if you can. If you claim you can do a certain measurement an xx% better, then also discuss how this will be relevant. The referee is generally not an expert in your field (but there will be one among the panel).

Proposal Form

EUROPEAN SOUTHERN OBSERVATORY Organisation Européenne pour des Recherches Astronomiques dans l Hémisphère Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre OBSERVING PROGRAMMES OFFICE Karl-Schwarzschild-Straße 2 D-85748 Garching bei München e-mail: opo@eso.org Tel. : +49-89-32 00 64 73 APPLICATION FOR OBSERVING TIME PERIOD: 89A Important Notice: By submitting this proposal, the PI takes full responsibility for the content of the proposal, in particular with regard to the names of CoIs and the agreement to act according to the ESO policy and regulations, should observing time be granted 1. Title Category: C 3 Soon to be accreted? Proper motions of gas near the black hole at the center of the Galaxy. 2. Abstract / Total Time Requested Total Amount of Time: 2 nights VM, 0 hours SM The massive black hole at the Galactic center is surrounded by a cluster of young, massive stars and several streamers of ionized, dusty gas. Within 2 of the black hole, at the bottom of the Galaxy s gravitational potential well, there are several dusty gas streams that are apparently undergoing interactions with the black hole. We propose to use the VISIR burst mode in combination with holographic image reconstruction to obtain precise, almost perfect MIR images of the GC. We already have a holographic image from 2007, which will provide a 5-yr time baseline. Stars with known positions and proper motions can be detected in the MIR, establishing an astrometric reference frame. We will thus be able to map the proper motions of the gas to address the following questions: Will some of the gas be accreted in coming decades? Can we find new evidence for dynamical interactions of the gas with a strong wind emanating from the vicinity of Sgr A*? 3. Run Period Instrument Time Month Moon Seeing Sky Mode Type A 89 VISIR 2n jun n n THN v 4. Number of nights/hours Telescope(s) Amount of time a) already awarded to this project: b) still required to complete this project: 5. Special remarks: This program could make e cient use of bad seeing conditions if the burst mode observations were carried out in service mode, but according to the CfP, burst mode is only o ered in visitor mode. 6. Principal Investigator: R. Schoedel, rainer@iaa.es, E, Instituto de Astrofisica de Andalucia (CSIC) 6a. Co-investigators: M. Morris University of California at Los Angeles,Department of Physics and Astronomy,US K. Muzic University of Toronto,Department of Astronomy and Astrophysics,CA 7. Is this proposal linked to a PhD thesis preparation? State role of PhD student in this project

EUROPEAN SOUTHERN OBSERVATORY Organisation Européenne pour des Recherches Astronomiques dans l Hémisphère Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre OBSERVING PROGRAMMES OFFICE Karl-Schwarzschild-Straße 2 D-85748 Garching bei München e-mail: opo@eso.org Tel. : +49-89-32 00 64 73 APPLICATION FOR OBSERVING TIME PERIOD: 89A Important Notice: By submitting this proposal, the PI takes full responsibility for the content of the proposal, in particular with regard to the names of CoIs and the agreement to act according to the ESO policy and regulations, should observing time be granted Does not matter, but please get it right. 1. Title Category: C 3 Soon to be accreted? Proper motions of gas near the black hole at the center of the Galaxy. 2. Abstract / Total Time Requested Total Amount of Time: 2 nights VM, 0 hours SM The massive black hole at the Galactic center is surrounded by a cluster of young, massive stars and several streamers of ionized, dusty gas. Within 2 of the black hole, at the bottom of the Galaxy s gravitational potential well, there are several dusty gas streams that are apparently undergoing interactions with the black hole. We propose to use the VISIR burst mode in combination with holographic image reconstruction to obtain precise, almost perfect MIR images of the GC. We already have a holographic image from 2007, which will provide a 5-yr time baseline. Stars with known positions and proper motions can be detected in the MIR, establishing an astrometric reference frame. We will thus be able to map the proper motions of the gas to address the following questions: Will some of the gas be accreted in coming decades? Can we find new evidence for dynamical interactions of the gas with a strong wind emanating from the vicinity of Sgr A*? 3. Run Period Instrument Time Month Moon Seeing Sky Mode Type A 89 VISIR 2n jun n n THN v 4. Number of nights/hours Telescope(s) Amount of time a) already awarded to this project: b) still required to complete this project: 5. Special remarks: This program could make e cient use of bad seeing conditions if the burst mode observations were carried out in service mode, but according to the CfP, burst mode is only o ered in visitor mode. 6. Principal Investigator: R. Schoedel, rainer@iaa.es, E, Instituto de Astrofisica de Andalucia (CSIC) 6a. Co-investigators: M. Morris University of California at Los Angeles,Department of Physics and Astronomy,US K. Muzic University of Toronto,Department of Astronomy and Astrophysics,CA 7. Is this proposal linked to a PhD thesis preparation? State role of PhD student in this project

EUROPEAN SOUTHERN OBSERVATORY Organisation Européenne pour des Recherches Astronomiques dans l Hémisphère Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre OBSERVING PROGRAMMES OFFICE Karl-Schwarzschild-Straße 2 D-85748 Garching bei München e-mail: opo@eso.org Tel. : +49-89-32 00 64 73 APPLICATION FOR OBSERVING TIME PERIOD: 89A Important Notice: Title should, above all, be clear and understandable (avoid abbreviations or very field-specific terms). By submitting this proposal, the PI takes full responsibility for the content of the proposal, in particular with regard to the names of CoIs and the agreement to act according to the ESO policy and regulations, should observing time be granted 1. Title Category: C 3 Soon to be accreted? Proper motions of gas near the black hole at the center of the Galaxy. 2. Abstract / Total Time Requested Total Amount of Time: 2 nights VM, 0 hours SM The massive black hole at the Galactic center is surrounded by a cluster of young, massive stars and several streamers of ionized, dusty gas. Within 2 of the black hole, at the bottom of the Galaxy s gravitational potential well, there are several dusty gas streams that are apparently undergoing interactions with the black hole. We propose to use the VISIR burst mode in combination with holographic image reconstruction to obtain precise, almost perfect MIR images of the GC. We already have a holographic image from 2007, which will provide a 5-yr time baseline. Stars with known positions and proper motions can be detected in the MIR, establishing an astrometric reference frame. We will thus be able to map the proper motions of the gas to address the following questions: Will some of the gas be accreted in coming decades? Can we find new evidence for dynamical interactions of the gas with a strong wind emanating from the vicinity of Sgr A*? 3. Run Period Instrument Time Month Moon Seeing Sky Mode Type A 89 VISIR 2n jun n n THN v 4. Number of nights/hours Telescope(s) Amount of time a) already awarded to this project: b) still required to complete this project: 5. Special remarks: This program could make e cient use of bad seeing conditions if the burst mode observations were carried out in service mode, but according to the CfP, burst mode is only o ered in visitor mode. 6. Principal Investigator: R. Schoedel, rainer@iaa.es, E, Instituto de Astrofisica de Andalucia (CSIC) 6a. Co-investigators: M. Morris University of California at Los Angeles,Department of Physics and Astronomy,US K. Muzic University of Toronto,Department of Astronomy and Astrophysics,CA 7. Is this proposal linked to a PhD thesis preparation? State role of PhD student in this project

EUROPEAN SOUTHERN OBSERVATORY Organisation Européenne pour des Recherches Astronomiques dans l Hémisphère Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre OBSERVING PROGRAMMES OFFICE Karl-Schwarzschild-Straße 2 D-85748 Garching bei München e-mail: opo@eso.org Tel. : +49-89-32 00 64 73 APPLICATION FOR OBSERVING TIME PERIOD: 89A Important Notice: By submitting this proposal, the PI takes full responsibility for the content of the proposal, in particular with regard to the names of CoIs and the agreement to act according to the ESO policy and regulations, should observing time be granted 1. Title Category: C 3 Soon to be accreted? Proper motions of gas near the black hole at the center of the Galaxy. 2. Abstract / Total Time Requested Total Amount of Time: 2 nights VM, 0 hours SM The massive black hole at the Galactic center is surrounded by a cluster of young, massive stars and several streamers of ionized, dusty gas. Within 2 of the black hole, at the bottom of the Galaxy s gravitational potential well, there are several dusty gas streams that are apparently undergoing interactions with the black hole. We propose to use the VISIR burst mode in combination with holographic image reconstruction to obtain precise, almost perfect MIR images of the GC. We already have a holographic image from 2007, which will provide a 5-yr time baseline. Stars with known positions and proper motions can be detected in the MIR, establishing an astrometric reference frame. We will thus be able to map the proper motions of the gas to address the following questions: Will some of the gas be accreted in coming decades? Can we find new evidence for dynamical interactions of the gas with a strong wind emanating from the vicinity of Sgr A*? 3. Run Period Instrument Time Month Moon Seeing Sky Mode Type A 89 VISIR 2n jun n n THN v VERY IMPORTANT. Must be clear, easy to understand, and make a convincing case. It is the first impression the referee gets from your proposal. Careful: Don t exceed the size of the box. 4. Number of nights/hours Telescope(s) Amount of time a) already awarded to this project: b) still required to complete this project: 5. Special remarks: This program could make e cient use of bad seeing conditions if the burst mode observations were carried out in service mode, but according to the CfP, burst mode is only o ered in visitor mode. 6. Principal Investigator: R. Schoedel, rainer@iaa.es, E, Instituto de Astrofisica de Andalucia (CSIC) 6a. Co-investigators: M. Morris University of California at Los Angeles,Department of Physics and Astronomy,US K. Muzic University of Toronto,Department of Astronomy and Astrophysics,CA 7. Is this proposal linked to a PhD thesis preparation? State role of PhD student in this project

EUROPEAN SOUTHERN OBSERVATORY Organisation Européenne pour des Recherches Astronomiques dans l Hémisphère Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre OBSERVING PROGRAMMES OFFICE Karl-Schwarzschild-Straße 2 D-85748 Garching bei München e-mail: opo@eso.org Tel. : +49-89-32 00 64 73 APPLICATION FOR OBSERVING TIME PERIOD: 89A Important Notice: By submitting this proposal, the PI takes full responsibility for the content of the proposal, in particular with regard to the names of CoIs and the agreement to act according to the ESO policy and regulations, should observing time be granted 1. Title Category: C 3 Soon to be accreted? Proper motions of gas near the black hole at the center of the Galaxy. 2. Abstract / Total Time Requested Total Amount of Time: 2 nights VM, 0 hours SM The massive black hole at the Galactic center is surrounded by a cluster of young, massive stars and several streamers of ionized, dusty gas. Within 2 of the black hole, at the bottom of the Galaxy s gravitational potential well, there are several dusty gas streams that are apparently undergoing interactions with the black hole. We propose to use the VISIR burst mode in combination with holographic image reconstruction to obtain precise, almost perfect MIR images of the GC. We already have a holographic image from 2007, which will provide a 5-yr time baseline. Stars with known positions and proper motions can be detected in the MIR, establishing an astrometric reference frame. We will thus be able to map the proper motions of the gas to address the following questions: Will some of the gas be accreted in coming decades? Can we find new evidence for dynamical interactions of the gas with a strong wind emanating from the vicinity of Sgr A*? 3. Run Period Instrument Time Month Moon Seeing Sky Mode Type A 89 VISIR 2n jun n n THN v 4. Number of nights/hours Telescope(s) Amount of time a) already awarded to this project: b) still required to complete this project: 5. Special remarks: This program could make e cient use of bad seeing conditions if the burst mode observations were carried out in service mode, but according to the CfP, burst mode is only o ered in visitor mode. 6. Principal Investigator: R. Schoedel, rainer@iaa.es, E, Instituto de Astrofisica de Andalucia (CSIC) 6a. Co-investigators: M. Morris University of California at Los Angeles,Department of Physics and Astronomy,US K. Muzic University of Toronto,Department of Astronomy and Astrophysics,CA VERY IMPORTANT. Requested time must coincide with time justification in Box 13. Request worst acceptable observing conditions. 7. Is this proposal linked to a PhD thesis preparation? State role of PhD student in this project

EUROPEAN SOUTHERN OBSERVATORY Organisation Européenne pour des Recherches Astronomiques dans l Hémisphère Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre OBSERVING PROGRAMMES OFFICE Karl-Schwarzschild-Straße 2 D-85748 Garching bei München e-mail: opo@eso.org Tel. : +49-89-32 00 64 73 APPLICATION FOR OBSERVING TIME PERIOD: 89A Important Notice: By submitting this proposal, the PI takes full responsibility for the content of the proposal, in particular with regard to the names of CoIs and the agreement to act according to the ESO policy and regulations, should observing time be granted 1. Title Category: C 3 Soon to be accreted? Proper motions of gas near the black hole at the center of the Galaxy. 2. Abstract / Total Time Requested Total Amount of Time: 2 nights VM, 0 hours SM The massive black hole at the Galactic center is surrounded by a cluster of young, massive stars and several streamers of ionized, dusty gas. Within 2 of the black hole, at the bottom of the Galaxy s gravitational potential well, there are several dusty gas streams that are apparently undergoing interactions with the black hole. We propose to use the VISIR burst mode in combination with holographic image reconstruction to obtain precise, almost perfect MIR images of the GC. We already have a holographic image from 2007, which will provide a 5-yr time baseline. Stars with known positions and proper motions can be detected in the MIR, establishing an astrometric reference frame. We will thus be able to map the proper motions of the gas to address the following questions: Will some of the gas be accreted in coming decades? Can we find new evidence for dynamical interactions of the gas with a strong wind emanating from the vicinity of Sgr A*? 3. Run Period Instrument Time Month Moon Seeing Sky Mode Type A 89 VISIR 2n jun n n THN v IMPORTANT: Time already awareded to this project or still necessary for completion after the present proposal. It is good if time has already been awarded, but in this case clearly state the obtained results in the scientific justification and whay you need more time. 4. Number of nights/hours Telescope(s) Amount of time a) already awarded to this project: b) still required to complete this project: 5. Special remarks: This program could make e cient use of bad seeing conditions if the burst mode observations were carried out in service mode, but according to the CfP, burst mode is only o ered in visitor mode. 6. Principal Investigator: R. Schoedel, rainer@iaa.es, E, Instituto de Astrofisica de Andalucia (CSIC) 6a. Co-investigators: M. Morris University of California at Los Angeles,Department of Physics and Astronomy,US K. Muzic University of Toronto,Department of Astronomy and Astrophysics,CA 7. Is this proposal linked to a PhD thesis preparation? State role of PhD student in this project

EUROPEAN SOUTHERN OBSERVATORY Organisation Européenne pour des Recherches Astronomiques dans l Hémisphère Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre OBSERVING PROGRAMMES OFFICE Karl-Schwarzschild-Straße 2 D-85748 Garching bei München e-mail: opo@eso.org Tel. : +49-89-32 00 64 73 APPLICATION FOR OBSERVING TIME PERIOD: 89A Important Notice: By submitting this proposal, the PI takes full responsibility for the content of the proposal, in particular with regard to the names of CoIs and the agreement to act according to the ESO policy and regulations, should observing time be granted 1. Title Category: C 3 Soon to be accreted? Proper motions of gas near the black hole at the center of the Galaxy. 2. Abstract / Total Time Requested Total Amount of Time: 2 nights VM, 0 hours SM The massive black hole at the Galactic center is surrounded by a cluster of young, massive stars and several streamers of ionized, dusty gas. Within 2 of the black hole, at the bottom of the Galaxy s gravitational potential well, there are several dusty gas streams that are apparently undergoing interactions with the black hole. We propose to use the VISIR burst mode in combination with holographic image reconstruction to obtain precise, almost perfect MIR images of the GC. We already have a holographic image from 2007, which will provide a 5-yr time baseline. Stars with known positions and proper motions can be detected in the MIR, establishing an astrometric reference frame. We will thus be able to map the proper motions of the gas to address the following questions: Will some of the gas be accreted in coming decades? Can we find new evidence for dynamical interactions of the gas with a strong wind emanating from the vicinity of Sgr A*? 3. Run Period Instrument Time Month Moon Seeing Sky Mode Type A 89 VISIR 2n jun n n THN v Special remarks (e.g.: proposal re-submission etc. ) 4. Number of nights/hours Telescope(s) Amount of time a) already awarded to this project: b) still required to complete this project: 5. Special remarks: This program could make e cient use of bad seeing conditions if the burst mode observations were carried out in service mode, but according to the CfP, burst mode is only o ered in visitor mode. 6. Principal Investigator: R. Schoedel, rainer@iaa.es, E, Instituto de Astrofisica de Andalucia (CSIC) 6a. Co-investigators: M. Morris University of California at Los Angeles,Department of Physics and Astronomy,US K. Muzic University of Toronto,Department of Astronomy and Astrophysics,CA 7. Is this proposal linked to a PhD thesis preparation? State role of PhD student in this project

8. Description of the proposed programme A Scientific Rationale: The dusty ISM in the vicinity of the Milky Way s massive black hole. The Milky Way s 4 10 6 M central black hole, Sagittarius A* (Sgr A*) is surrounded by a nuclear cluster of old stars and a group of massive, young stars within 0.5 pc (e.g., Genzel+ 2010). Sagittarius A West, the so-called mini-spiral, is a prominent feature of the interstellar-medium (ISM) in the inner 2 pc (Ekers+ 1983, Lo & Claussen 1983). It is roughly made up of three streamers of ionized gas, termed the Northern, Western, and Eastern arms, that are ionized by the radiation from the young stars. The overall dynamics of the mini-spiral can be described by three bundles of quasi-keplerian orbits (e.g., Paumard+ 2004, Zhao+ 2009). The gas is accompanied by warm dust, and adaptive optics observations at 3.8 µm with NACO/VLT and at 8.6 µm with VISIR/VLT have revealed an impressive amount of detail in the mini-spiral (e.g., Muzic+ 2007; Viehmann+ 2006, Schödel+ 2011; Figs. 1-4). One of the most interesting aspects of these gas streams is that they are destined to lead to accretion episodes onto Sgr A* on time scales of 10 3-10 4 years. Morphology and kinematics of the mini-spiral near Sgr A*. The dusty ISM within a few 0.1 pc of Sgr A* shows an impressively complex morphology, but certain general patterns can be observed: for one, the numerous thin filamentary structures are almost all oriented with their concave sides facing Sgr A*. Muzic+ (2007, Fig. 1) measured the (perpendicular) proper motion of parts of several of these filaments in 3.8 µm NACO images and found that they are generally directed away from Sgr A*. They interpret these patterns in terms of a strong outflow from the center, but cannot say whether it originates from the stars, Sgr A*, or both. Two cometary-shaped sources close to Sgr A* X3 and X7 provide further evidence of an outflow from the direction of Sgr A* (Muzic+ 2010; X7 shown in Fig. 2). This outflow appears to be directed NE-SW and points toward the mini-cavity, a well-defined cavity in the ISM, about 0.2 pc SW of Sgr A* (Fig. 1+3, Yusef-Zadeh & Wardle 1993; Lutz+ 1993). Zhao+ (2009) examined VLA measurements of the mini-spiral and derived proper motions for a large number of features in this HII region. Their findings agree with the overall picture described above. MIR imaging of the Galactic center with VISIR. Observing the morphology and, particularly, measuring the proper motions of the ISM at 3.8 µm isverydi cult because of confusion with stars in the dense cluster (Fig. 1, Muzic+ 2007). Radio images, on the other hand, su er from the high brightness of Sgr A* at these wavelengths and cannot provide much information in the central arcsecond (Zhao+ 2009). The mid-infrared therefore provides the optimal view of the mini-spiral and its structures because both the stars and Sgr A* are very faint there, while the dust is bright (Figs. 2-4, Viehmann+ 2006, Schödel+ 2011). Detailed features of the ISM can be observed within just 2 (0.08 pc in projection) of Sgr A*, which show up clearly only in MIR images. Among the closest such structures to SgrA*, several have a finger-like morphology, pointing toward Sgr A* (Fig. 2; Schödel+ 2011), strongly suggestive of accreting gas streams with infall times of mere decades. They are presumably shaped by tidal stretching of infalling gas clumps, as they accelerate toward the black hole. If so, the proper motion in the MIR should be readily observable, and allow us to model their subsequent future motion as they stream toward their dramatic destiny. Another intriguing structure is the IR ridge underlying Sgr A* (Fig. 2, Schödel+ 2011). If this ridge is physically close to Sgr A*, then it would have a high proper motion, and would very soon lead to accretion onto the black hole. As concerns the filaments we expect more detailed proper motions than what could be done in the L 0 - band (Fig. 1, Muzic+ 2007) because we will not be limited to fields with low stellar confusion. We thus only have to address the question of feasibility. Measuring proper motions of the ISM with VISIR: Yes, we can! In Schödel+ 2011 we show how almost perfect images can be reconstructed from VISIR burst mode data through holographic reconstruction, using the bright star IRS 3 as reference. In Fig. 4, two images (nights 22/23 May and 7/8 April 2007; Schödel+ 2011) from two completely independent data sets, obtained under 2 and 0.7 visual seeing, are compared. No significant di erence can be seen between the images. The right panel of Fig. 4 shows the clear signal that is obtained after shifting the April 2007 image by 0.25 pixels and subtracting it from the May 2007 image. The proper motions found by Muzic+ (2007) are on the order of 200 km/s. Furthermore, the stellar velocity dispersion at 1 projected distance from Sgr A* is 200 km/s (Schödel+ 2009), which correspond to 0.04 mas/yr at a distance of 8 kpc. We have a deep, holographic image from a combination of all 8.6 µm 2007 burst mode data (Figs. 2-4, Schödel+ 2011), so on a five-year (2007-2012) time baseline we can therefore expect positional shifts of 20 mas, or roughly 0.25 pixels on the old VISIR detector. From Fig. 4 there remains no doubt that such small proper motions 200 km/s can be detected. Moreover, a significant number of stars can be detected in the MIR images ( IRS sources, Figs. 2+3). Their precisely known positions and proper motions (Schödel+ 2009) establish an accurate astrometric reference frame. The members of our team have ample experience with high-precision proper motion measurements of both stars and extended features (Muzic+ 2007; Schödel+ 2009). B ImmediateObjective: Our immediate objectives are to obtain a deep, high-strehl PAH1 image of the surroundings of Sgr A* with VISIR, using burst mode, and then to apply holographic image reconstruction. The new image from the 2012 epoch will be used to infer the proper motions of the ISM features in the minispiral, with particular attention to the region within 2 arcseconds of Sgr A*, where dust streams are likely to be descending toward a self-imposed inferno. A comparison with the 2007 image will also enable us to set fundamental constraints on the long-term variability of the emission from Sgr A* at 8.6 µm (Schödel+ 2011). 8. Description of the proposed programme and attachments mini spiral Northern Arm Fig. 1: Proper motions of filaments Fig. 2: Environment of Sgr A* mini cavity Fig. 3: Holographic imaging IRS7 IRS9 single exposure long exposure SSA Holography Fig. 4: Measuring proper motions of the ISM 22/23 May 2007 IRS21 IRS3 IRS6E IRS 16NW IRS29N IRS16C 7/8 April 2007 difference after 0.25 pix shift SgrA* Ridge X7 mini cavity Fig. 1: The mini-spiral in the GC. L 0 -band (3.8 µm) image from NACO with proper motions of some filaments indicated, as measured by Muzic+ (2007). Fig. 2: Close up of the surroundings of Sgr A* at 8.6 µm. Image from a combined holographic reduction of all VISIR PAH1 burst mode data from 2007 (Schödel+ 2011). The cross at (0, 0 ) marks the position of Sgr A*, which sits right atop a dust ridge. Contour lines are plotted in steps of 0.5 mjy from 0.5 to 20 mjy per pixel (0.075 per pixel scale). Great detail in the MIR emission is visible. Most of it is due to compact dust features (IRS16NW, IRS16C, IRS29N are stars). Fig. 3: Holographic imaging of the GC with VISIR. Burst mode data on the GC were obtained with VISIR (PAH1) on 23 May 2007 under 2 visual seeing. From left to right: Single short-exposure frame. Tip-tilt corrected long exposure. Traditional simple shift-and-add (SSA) image reconstruction. Holographic imaging, using IRS 3, the brightest source in the image, as reference. The Strehl ratio is > 90%. Note that the extended emission around IRS 3 is no problem for the holographic technique because the di use emission lies below the noise-cut o in the individual frames. Fig. 4: PSF stability and the possibility to measure proper motions of dusty features in the GC. The left and middle images are holographic reconstructions of the VISIR PAH1 burst mode images from 22/23 May and 7/8 April 2007, which were acquired under completely di erent seeing conditions: 2 (May) and 0.7 (April). Nevertheless, the Strehl ratio of both reconstructed images is > 90%. Holographic imaging of the GC is superior to standard imaging in terms of image sharpness/psf stability under all but the most exceptional seeing conditions. The right panel shows the di erence between the two images after shifting one of them by just 0.25 pixel, corresponding to the displacement of a feature with 200 km/s proper motion after 5 yr. References in addition to Box 11: Ekers+ 1983, A&A, 122, 143. Genzel+ 2010, Rev. Mod. Phys., 82, 3121-3195. Lo & Claussen 1983, Nature, 306, 647. Lutz+ 1993, ApJ, 418, 244. Muzic+ 2007, A&A, 469, 993-1002. Paumard+ 2004, A&A, 426, 81. Schödel+ 2007, A&A, 462, L1-L4. Viehmann+ 2006, ApJ, 642, 861-867. Yusef-Zadeh & Wardle 1993, ApJ, 405, 584. Zhao, Morris+ 2009, ApJ, 699, 186-214.

8. Description of the proposed programme B ImmediateObjective: Our immediate objectives are to obtain a deep, high-strehl PAH1 image of the surroundings of Sgr A* with VISIR, using burst mode, and then to apply holographic image reconstruction. The new image from the 2012 epoch will be used to infer the proper motions of the ISM features in the minispiral, with particular attention to the region within 2 arcseconds of Sgr A*, where dust streams are likely to be descending toward a self-imposed inferno. A comparison with the 2007 image will also enable us to set fundamental constraints on the long-term variability of the emission from Sgr A* at 8.6 µm (Schödel+ 2011). 8. Description of the proposed programme and attachments Fig. 1: Proper motions of filaments A Scientific Rationale: Fig. 2: Environment of Sgr A* The dusty ISM in the vicinity of the Milky Way s massive black hole. The Milky Way s 4 10 6 IRS 16NW THE M central black DECISIVE hole, Sagittarius A* (Sgr A*) is surrounded PART. by a nuclear cluster of old stars and a group IRS29N of massive, young stars within 0.5 pc (e.g., Genzel+ 2010). Sagittarius A West, the so-called mini-spiral, is a prominent feature of the interstellar-medium (ISM) in the inner 2 pc (Ekers+ 1983, Lo & Claussen 1983). It IRS16C is roughly made up of three streamers of ionized gas, termed the Northern, Western, and Eastern arms, that SgrA* Ridge are ionized by the radiation from the young stars. The overall dynamics of the mini-spiral can be described mini spiral by three bundles of quasi-keplerian orbits (e.g., Paumard+ 2004, Zhao+ 2009). The gas is accompanied by Northern Arm warm dust, and adaptive optics observations at 3.8 µm with NACO/VLT and at 8.6 µm with VISIR/VLT have revealed an impressive amount of detail in the mini-spiral (e.g., Muzic+ 2007; Viehmann+ 2006, Schödel+ X7 For a normal proposal, you have a maximum of 2 pages for the 2011; Figs. 1-4). One of the most interesting aspects of these gas streams is that they are destined to lead to accretion episodes onto Sgr A* on time scales of 10 3-10 4 years. Morphology and kinematics of the mini-spiral near Sgr A*. The dusty ISM within a few 0.1 pc of mini cavity Sgr scientific A* shows an impressively complex justification morphology, but certain general patterns, can including be observed: for one, the figures and references (except Fig. 3: Holographic imaging numerous thin filamentary structures are almost all oriented with their concave sides facing Sgr A*. Muzic+ single exposure long exposure SSA Holography (2007, Fig. 1) measured the (perpendicular) proper motion of parts of several of these filaments 3.8 µm NACO images and found that they are generally directed away from Sgr A*. They interpret these patterns in terms your most recent ones, which are contained in Box 11). of a strong outflow from the center, but cannot say whether it originates from the stars, Sgr A*, or both. Two cometary-shaped sources close to Sgr A* X3 and X7 provide further evidence of an outflow from the direction of Sgr A* (Muzic+ 2010; X7 shown in Fig. 2). This outflow appears to be directed NE-SW and points toward the mini-cavity, a well-defined cavity in the ISM, about 0.2 pc SW of Sgr A* (Fig. 1+3, Yusef-Zadeh & Wardle 1993; Lutz+ 1993). Zhao+ (2009) examined VLA measurements of the mini-spiral and derived proper motions for a large number of features in this HII region. Their findings agree with the overall picture described above. mini cavity MIR imaging of the Galactic center with VISIR. Observing the morphology and, particularly, measuring the The proper motions length of the ISM at 3.8 µm of isverydi the cult because justification of confusion with stars in the dense cluster is not a good Fig. 4: Measuring measure proper motions of the of ISM its quality. (Fig. 1, Muzic+ 2007). Radio images, on the other hand, su er from the high brightness of Sgr A* these 22/23 May 2007 7/8 April 2007 difference after 0.25 pix shift wavelengths and cannot provide much information in the central arcsecond (Zhao+ 2009). The mid-infrared IRS7 therefore provides the optimal view of the mini-spiral and its structures because both the stars and Sgr A* are IRS3 very faint there, while the dust is bright (Figs. 2-4, Viehmann+ 2006, Schödel+ 2011). Detailed features of the ISM can be observed within just 2 (0.08 pc in projection) of Sgr A*, which show up clearly only in MIR images. Among the closest such structures to SgrA*, several have a finger-like morphology, pointing toward Sgr Each A* (Fig. 2; Schödel+ referee 2011), strongly suggestive may of accreting only gas streams with read infall times of this mere decades. once, so it is very IRS6E important to use They are presumably shaped by tidal stretching of infalling gas clumps, as they accelerate toward the black hole. If so, the proper motion in the MIR should be readily observable, and allow us to model their subsequent future IRS9 IRS21 motion as they stream toward their dramatic destiny. Another intriguing structure is the IR ridge underlying a clear structure and language and clear, Sgr A* (Fig. 2, Schödel+ 2011). If this ridge is physically close to Sgr A*, then it would have a high proper Fig. 1: The mini-spiral in the GC. L 0 concrete -band (3.8 µm) image from NACO with proper motions of some motion, and would very soon lead to accretion onto the black hole. As concerns the filaments we expect more filaments indicated, as measured by Muzic+ (2007). Fig. 2: Close up of the surroundings of Sgr A* at detailed proper motions than what could be done in the L 0 - band (Fig. 1, Muzic+ 2007) because we will not be 8.6 µm. Image from a combined holographic reduction of all VISIR PAH1 burst mode data from 2007 (Schödel+ limited goals. to fields with low stellar confusion. We thus only have to address the question of feasibility. 2011). The cross at (0, 0 ) marks the position of Sgr A*, which sits right atop a dust ridge. Contour lines Measuring proper motions of the ISM with VISIR: Yes, we can! In Schödel+ 2011 we show how almost are plotted in steps of 0.5 mjy from 0.5 to 20 mjy per pixel (0.075 per pixel scale). Great detail in the MIR perfect images can be reconstructed from VISIR burst mode data through holographic reconstruction, using the emission is visible. Most of it is due to compact dust features (IRS16NW, IRS16C, IRS29N are stars). bright star IRS 3 as reference. In Fig. 4, two images (nights 22/23 May and 7/8 April 2007; Schödel+ 2011) from Fig. 3: Holographic imaging of the GC with VISIR. Burst mode data on the GC were obtained with two completely independent data sets, obtained under 2 and 0.7 visual seeing, are compared. No significant VISIR (PAH1) on 23 May 2007 under 2 visual seeing. From left to right: Single short-exposure frame. di erence can be seen between the images. The right panel of Fig. 4 shows the clear signal that is obtained after shifting the April 2007 image by 0.25 pixels and subtracting it from the May 2007 image. The proper Tip-tilt corrected long exposure. Traditional simple shift-and-add (SSA) image reconstruction. Holographic imaging, using IRS 3, the brightest source in the image, as reference. The Strehl ratio is > 90%. Note that the motions Figures found by Muzic+ (2007) can are on the be order of very 200 km/s. Furthermore, helpful, the stellar velocity but dispersion are extended not emission around necessary. IRS 3 is no problem for the holographic technique because the di use emission lies at 1 projected distance from Sgr A* is 200 km/s (Schödel+ 2009), which correspond to 0.04 mas/yr at a below the noise-cut o in the individual frames. distance of 8 kpc. We have a deep, holographic image from a combination of all 8.6 µm 2007 burst mode data Fig. 4: PSF stability and the possibility to measure proper motions of dusty features in the GC. (Figs. 2-4, Schödel+ 2011), so on a five-year (2007-2012) time baseline we can therefore expect positional shifts of 20 mas, or roughly 0.25 pixels on the old VISIR detector. From Fig. 4 there remains no doubt that such The left and middle images are holographic reconstructions of the VISIR PAH1 burst mode images from 22/23 May and 7/8 April 2007, which were acquired under completely di erent seeing conditions: 2 (May) and 0.7 small proper motions 200 km/s can be detected. Moreover, a significant number of stars can be detected in (April). Nevertheless, the Strehl ratio of both reconstructed images is > 90%. Holographic imaging of the GC the MIR images ( IRS sources, Figs. 2+3). Their precisely known positions and proper motions (Schödel+ 2009) establish an accurate astrometric reference frame. The members of our team have ample experience with high-precision proper motion measurements of both stars and extended features (Muzic+ 2007; Schödel+ 2009). is superior to standard imaging in terms of image sharpness/psf stability under all but the most exceptional seeing conditions. The right panel shows the di erence between the two images after shifting one of them by just 0.25 pixel, corresponding to the displacement of a feature with 200 km/s proper motion after 5 yr. Make sure that your figures convey a clear message and that References in addition to Box 11: Ekers+ 1983, A&A, 122, 143. Genzel+ 2010, Rev. Mod. Phys., 82, 3121-3195. Lo & Claussen 1983, Nature, 306, 647. Lutz+ 1993, ApJ, 418, 244. Muzic+ 2007, A&A, 469, 993-1002. Paumard+ 2004, A&A, 426, 81. Schödel+ 2007, A&A, 462, L1-L4. Viehmann+ 2006, ApJ, 642, 861-867. Yusef-Zadeh & Wardle 1993, ApJ, 405, 584. Zhao, Morris+ 2009, ApJ, 699, 186-214. they are of sufficient quality (avoid too small labels on axes...)

9. Justification of requested observing time and observing conditions Lunar Phase Justification: No restrictions. Time Justification: (including seeing overhead) Our goal is ro obtain a deep, accurate image of the GC at 8.6 µm and to image features as faint as 100 mjy arcsec 2 with a S/N > 10 with extremely high Strehl ratio. Only burst mode observations combined with holographic image reconstruction can guarantee the degree of image stability that we require. We have ample experience in MIR imaging of the GC with VISIR (with and without burst mode, Viehmann+ 2006, Schödel+ 2007, Schödel+ 2011). The main issue that has to be addressed in MIR imaging of the GC is that the target is extended. The region around Sgr A* is dominated on scales of 30 by emission from the bright mini-spiral. Chopping and nodding have to be done o -source, leading to an overhead of a factor 4, compared to observations of a point source with VISIR. Also, burst mode observations are more ine cient than standard imaging with VISIR because the data pipeline is not able to handle the high data rate, which leads to frame loss, adding another factor 3 to the overhead (see Schödel+ 2011). Care has to be taken to optimize chopping and dithering. While chopping toward the NW typically provides the best choice, there is no chopping angle and o set that can guarantee the image to be free of residuals. It is therefore imperative to acquire images at several dither positions and with di erent chopping angles and directions to minimize systematic errors. Our goal is a 8.6 µm image at least as good as the sum-image from all 2007 data. The 2007 image (see Schödel+ 2011) comprises 4.5 h of e ective on-source integration, from a total of 12 epochs of observation, which makes up about full 2 nights because of the overheads described above. 9a. Telescope Justification: There is no alternative. Compared to other existing MIR instruments at large telescopes, the burst mode of VISIR provides an enormous advantage for observations of the GC because it guarantees close to perfect image quality through the application of holographic image reconstruction (Schödel+ 2011). 9b. Observing Mode Justification (visitor or service): The burst mode is only o ered in visitor mode. We would happily accept service mode. Note that the suggested observations will work with seeing up to 2 and could therefore be used to e ciently make use of bad nights on Paranal. According to the instrument scientist and the CfP service mode is not o ered with burst mode, unfortunately, not even for observers experienced with the setup. 9c. Calibration Request: Standard Calibration

9. Justification of requested observing time and observing conditions Lunar Phase Justification: No restrictions. Time Justification: (including seeing overhead) Our goal is ro obtain a deep, accurate image of the GC at 8.6 µm and to image features as faint as 100 mjy arcsec 2 with a S/N > 10 with extremely high Strehl ratio. Only burst mode observations combined with holographic image reconstruction can guarantee the degree of image stability that we require. We have ample experience in MIR imaging of the GC with VISIR (with and without burst mode, Viehmann+ 2006, Schödel+ 2007, Schödel+ 2011). The main issue that has to be addressed in MIR imaging of the GC is that the target is extended. The region around Sgr A* is dominated on scales of 30 by emission from the bright mini-spiral. Chopping and nodding have to be done o -source, leading to an overhead of a factor 4, compared to observations of a point source with VISIR. Also, burst mode observations are more ine cient than standard imaging with VISIR because the data pipeline is not able to handle the high data rate, which leads to frame loss, adding another factor 3 to the overhead (see Schödel+ 2011). Care has to be taken to optimize chopping and dithering. While chopping toward the NW typically provides the best choice, there is no chopping angle and o set that can guarantee the image to be free of residuals. It is therefore imperative to acquire images at several dither positions and with di erent chopping angles and directions to minimize systematic errors. Our goal is a 8.6 µm image at least as good as the sum-image from all 2007 data. The 2007 image (see Schödel+ 2011) comprises 4.5 h of e ective on-source integration, from a total of 12 epochs of observation, which makes up about full 2 nights because of the overheads described above. Important. Make a clear justification of the requested time, including overheads. 9a. Telescope Justification: There is no alternative. Compared to other existing MIR instruments at large telescopes, the burst mode of VISIR provides an enormous advantage for observations of the GC because it guarantees close to perfect image quality through the application of holographic image reconstruction (Schödel+ 2011). 9b. Observing Mode Justification (visitor or service): The burst mode is only o ered in visitor mode. We would happily accept service mode. Note that the suggested observations will work with seeing up to 2 and could therefore be used to e ciently make use of bad nights on Paranal. According to the instrument scientist and the CfP service mode is not o ered with burst mode, unfortunately, not even for observers experienced with the setup. 9c. Calibration Request: Standard Calibration

9. Justification of requested observing time and observing conditions Lunar Phase Justification: No restrictions. Time Justification: (including seeing overhead) Our goal is ro obtain a deep, accurate image of the GC at 8.6 µm and to image features as faint as 100 mjy arcsec 2 with a S/N > 10 with extremely high Strehl ratio. Only burst mode observations combined with holographic image reconstruction can guarantee the degree of image stability that we require. We have ample experience in MIR imaging of the GC with VISIR (with and without burst mode, Viehmann+ 2006, Schödel+ 2007, Schödel+ 2011). The main issue that has to be addressed in MIR imaging of the GC is that the target is extended. The region around Sgr A* is dominated on scales of 30 by emission from the bright mini-spiral. Chopping and nodding have to be done o -source, leading to an overhead of a factor 4, compared to observations of a point source with VISIR. Also, burst mode observations are more ine cient than standard imaging with VISIR because the data pipeline is not able to handle the high data rate, which leads to frame loss, adding another factor 3 to the overhead (see Schödel+ 2011). Care has to be taken to optimize chopping and dithering. While chopping toward the NW typically provides the best choice, there is no chopping angle and o set that can guarantee the image to be free of residuals. It is therefore imperative to acquire images at several dither positions and with di erent chopping angles and directions to minimize systematic errors. Our goal is a 8.6 µm image at least as good as the sum-image from all 2007 data. The 2007 image (see Schödel+ 2011) comprises 4.5 h of e ective on-source integration, from a total of 12 epochs of observation, which makes up about full 2 nights because of the overheads described above. 9a. Telescope Justification: There is no alternative. Compared to other existing MIR instruments at large telescopes, the burst mode of VISIR provides an enormous advantage for observations of the GC because it guarantees close to perfect image quality through the application of holographic image reconstruction (Schödel+ 2011). 9b. Observing Mode Justification (visitor or service): The burst mode is only o ered in visitor mode. We would happily accept service mode. Note that the suggested observations will work with seeing up to 2 and could therefore be used to e ciently make use of bad nights on Paranal. According to the instrument scientist and the CfP service mode is not o ered with burst mode, unfortunately, not even for observers experienced with the setup. Important. In particular if there are alternatives, provide a clear argument for the need of the requested telescope. 9c. Calibration Request: Standard Calibration

9. Justification of requested observing time and observing conditions Lunar Phase Justification: No restrictions. Time Justification: (including seeing overhead) Our goal is ro obtain a deep, accurate image of the GC at 8.6 µm and to image features as faint as 100 mjy arcsec 2 with a S/N > 10 with extremely high Strehl ratio. Only burst mode observations combined with holographic image reconstruction can guarantee the degree of image stability that we require. We have ample experience in MIR imaging of the GC with VISIR (with and without burst mode, Viehmann+ 2006, Schödel+ 2007, Schödel+ 2011). The main issue that has to be addressed in MIR imaging of the GC is that the target is extended. The region around Sgr A* is dominated on scales of 30 by emission from the bright mini-spiral. Chopping and nodding have to be done o -source, leading to an overhead of a factor 4, compared to observations of a point source with VISIR. Also, burst mode observations are more ine cient than standard imaging with VISIR because the data pipeline is not able to handle the high data rate, which leads to frame loss, adding another factor 3 to the overhead (see Schödel+ 2011). Care has to be taken to optimize chopping and dithering. While chopping toward the NW typically provides the best choice, there is no chopping angle and o set that can guarantee the image to be free of residuals. It is therefore imperative to acquire images at several dither positions and with di erent chopping angles and directions to minimize systematic errors. Our goal is a 8.6 µm image at least as good as the sum-image from all 2007 data. The 2007 image (see Schödel+ 2011) comprises 4.5 h of e ective on-source integration, from a total of 12 epochs of observation, which makes up about full 2 nights because of the overheads described above. 9a. Telescope Justification: There is no alternative. Compared to other existing MIR instruments at large telescopes, the burst mode of VISIR provides an enormous advantage for observations of the GC because it guarantees close to perfect image quality through the application of holographic image reconstruction (Schödel+ 2011). 9b. Observing Mode Justification (visitor or service): The burst mode is only o ered in visitor mode. We would happily accept service mode. Note that the suggested observations will work with seeing up to 2 and could therefore be used to e ciently make use of bad nights on Paranal. According to the instrument scientist and the CfP service mode is not o ered with burst mode, unfortunately, not even for observers experienced with the setup. Not relevant for evaluation by panel (but argue well if you want visitor mdoe). 9c. Calibration Request: Standard Calibration

9. Justification of requested observing time and observing conditions Lunar Phase Justification: No restrictions. Time Justification: (including seeing overhead) Our goal is ro obtain a deep, accurate image of the GC at 8.6 µm and to image features as faint as 100 mjy arcsec 2 with a S/N > 10 with extremely high Strehl ratio. Only burst mode observations combined with holographic image reconstruction can guarantee the degree of image stability that we require. We have ample experience in MIR imaging of the GC with VISIR (with and without burst mode, Viehmann+ 2006, Schödel+ 2007, Schödel+ 2011). The main issue that has to be addressed in MIR imaging of the GC is that the target is extended. The region around Sgr A* is dominated on scales of 30 by emission from the bright mini-spiral. Chopping and nodding have to be done o -source, leading to an overhead of a factor 4, compared to observations of a point source with VISIR. Also, burst mode observations are more ine cient than standard imaging with VISIR because the data pipeline is not able to handle the high data rate, which leads to frame loss, adding another factor 3 to the overhead (see Schödel+ 2011). Care has to be taken to optimize chopping and dithering. While chopping toward the NW typically provides the best choice, there is no chopping angle and o set that can guarantee the image to be free of residuals. It is therefore imperative to acquire images at several dither positions and with di erent chopping angles and directions to minimize systematic errors. Our goal is a 8.6 µm image at least as good as the sum-image from all 2007 data. The 2007 image (see Schödel+ 2011) comprises 4.5 h of e ective on-source integration, from a total of 12 epochs of observation, which makes up about full 2 nights because of the overheads described above. 9a. Telescope Justification: There is no alternative. Compared to other existing MIR instruments at large telescopes, the burst mode of VISIR provides an enormous advantage for observations of the GC because it guarantees close to perfect image quality through the application of holographic image reconstruction (Schödel+ 2011). 9b. Observing Mode Justification (visitor or service): The burst mode is only o ered in visitor mode. We would happily accept service mode. Note that the suggested observations will work with seeing up to 2 and could therefore be used to e ciently make use of bad nights on Paranal. According to the instrument scientist and the CfP service mode is not o ered with burst mode, unfortunately, not even for observers experienced with the setup. 9c. Calibration Request: Standard Calibration Not relevant for evaluation by panel. But make sure you request any necessary special calibrations.

10. Report on the use of ESO facilities during the last 2 years P85: 085.D-0214: 2 nights of visitor mode time at NACO (PI Schödel) for sparse aperture masking (SAM) interferometry on selected targets in the Galactic center, scheduled for 1-5 June 2010. Weather loss 50%, 20% low data quality because of extremely short atmospheric coherence time and low AO performance. 30% acceptable to good data quality. Analysis under way as part of PhD project of J. Sánchez. Preliminary results and a new way of auto-calibrating SAM data on dense clusters were presented by J. Sánchez at the conference Astrophysics at high angular resolution 2011 on 30 Aug 2011, in Bad Honnef, Germany. Publication in preparation. 485.L-0122: 5 hours of service mode time (PI Schödel) to determine an astrometric flat field for the NACO S27 camera with milliarcsecond accuracy. Data received in August 2010, analysis in progress, but very di cult because the service mode data were taken under extremely fast seeing with extremely small isoplanatic angle. This means that precision photometry across the S27 FOV is complicated because of the low Strehl ratio and spatially highly variable PSF. P87: 087.B-0658: 4h of service mode time on NACO (PI Schödel) for speckle holography of the Galactic center. Data acquired in August 2011. High-quality, high-strehl images were reconstructed from the data. Paper in preparation. 10a. ESO Archive - Are the data requested by this proposal in the ESO Archive (http://archive.eso.org)? If so, explain the need for new data. The requested data are NOT on the ESO Archive. 10b. GTO/Public Survey Duplications: 11. Applicant s publications related to the subject of this application during the last 2 years García-Marín, M.; Eckart, A.; Weiss, A.; Witzel, G.; Bremer, M.; Zamaninasab, M.; Morris, M. R.; Schödel, R. et al. 2011, ApJ, 738, article id.158: Extended Submillimeter Emission of the Galactic Center and Nearinfrared/submillimeter Variability of Its Supermassive Black Hole R. Schödel, M. R. Morris, K. Muzic, A. Alberdi, L. Meyer, A. Eckart & D. Y. Gezari 2011, A&A, 537, id.a83: The mean infrared emission of Sagittarius A* Girard J. H., Kasper M., Quanz S. P., Kenworthy M. A., Rengaswamy S., Schödel R. et al., 2010, Proceedings of the SPIE, 7736, 77362N: Status and new operation modes of the versatile VLT/NaCo Muzic K., Eckart A., Schoedel R., Buchholz R., Zamaninasab M., 2010, A&A, 521, A13: Cometary shaped sources at the Galactic Center - Evidence for a wind from the central 0.2 pc Schödel R., 2010, A&A, 509, A26: Accurate photometry with adaptive optics in the presence of anisoplanatic e ects with a sparsely sampled PSF. The Galactic center as an example of a challenging target for accurate AO photometry Schoedel R., Najarro F., Muzic K., Eckart A., 2010, A&A, 511, A18: Peering through the veil: near-infrared photometry and extinction for the Galactic nuclear star cluster. Accurate near infrared H, Ks, and L photometry and the near-infrared extinction-law toward the central parsec of the Galaxy Schödel R., Merritt D. & Eckart A., 2009, A& A, 503, 91-111: The nuclear star cluster of the Milky Way: proper motions and mass

10. Report on the use of ESO facilities during the last 2 years P85: 085.D-0214: 2 nights of visitor mode time at NACO (PI Schödel) for sparse aperture masking (SAM) interferometry on selected targets in the Galactic center, scheduled for 1-5 June 2010. Weather loss 50%, 20% low data quality because of extremely short atmospheric coherence time and low AO performance. 30% acceptable to good data quality. Analysis under way as part of PhD project of J. Sánchez. Preliminary results and a new way of auto-calibrating SAM data on dense clusters were presented by J. Sánchez at the conference Astrophysics at high angular resolution 2011 on 30 Aug 2011, in Bad Honnef, Germany. Publication in preparation. 485.L-0122: 5 hours of service mode time (PI Schödel) to determine an astrometric flat field for the NACO S27 camera with milliarcsecond accuracy. Data received in August 2010, analysis in progress, but very di cult because the service mode data were taken under extremely fast seeing with extremely small isoplanatic angle. This means that precision photometry across the S27 FOV is complicated because of the low Strehl ratio and spatially highly variable PSF. P87: 087.B-0658: 4h of service mode time on NACO (PI Schödel) for speckle holography of the Galactic center. Data acquired in August 2011. High-quality, high-strehl images were reconstructed from the data. Paper in preparation. Hardly relevant for evaluation by panel. If you list previous observations, it is good if you can point to a publication. 10a. ESO Archive - Are the data requested by this proposal in the ESO Archive (http://archive.eso.org)? If so, explain the need for new data. The requested data are NOT on the ESO Archive. 10b. GTO/Public Survey Duplications: 11. Applicant s publications related to the subject of this application during the last 2 years García-Marín, M.; Eckart, A.; Weiss, A.; Witzel, G.; Bremer, M.; Zamaninasab, M.; Morris, M. R.; Schödel, R. et al. 2011, ApJ, 738, article id.158: Extended Submillimeter Emission of the Galactic Center and Nearinfrared/submillimeter Variability of Its Supermassive Black Hole R. Schödel, M. R. Morris, K. Muzic, A. Alberdi, L. Meyer, A. Eckart & D. Y. Gezari 2011, A&A, 537, id.a83: The mean infrared emission of Sagittarius A* Girard J. H., Kasper M., Quanz S. P., Kenworthy M. A., Rengaswamy S., Schödel R. et al., 2010, Proceedings of the SPIE, 7736, 77362N: Status and new operation modes of the versatile VLT/NaCo Muzic K., Eckart A., Schoedel R., Buchholz R., Zamaninasab M., 2010, A&A, 521, A13: Cometary shaped sources at the Galactic Center - Evidence for a wind from the central 0.2 pc Schödel R., 2010, A&A, 509, A26: Accurate photometry with adaptive optics in the presence of anisoplanatic e ects with a sparsely sampled PSF. The Galactic center as an example of a challenging target for accurate AO photometry Schoedel R., Najarro F., Muzic K., Eckart A., 2010, A&A, 511, A18: Peering through the veil: near-infrared photometry and extinction for the Galactic nuclear star cluster. Accurate near infrared H, Ks, and L photometry and the near-infrared extinction-law toward the central parsec of the Galaxy Schödel R., Merritt D. & Eckart A., 2009, A& A, 503, 91-111: The nuclear star cluster of the Milky Way: proper motions and mass

10. Report on the use of ESO facilities during the last 2 years P85: 085.D-0214: 2 nights of visitor mode time at NACO (PI Schödel) for sparse aperture masking (SAM) interferometry on selected targets in the Galactic center, scheduled for 1-5 June 2010. Weather loss 50%, 20% low data quality because of extremely short atmospheric coherence time and low AO performance. 30% acceptable to good data quality. Analysis under way as part of PhD project of J. Sánchez. Preliminary results and a new way of auto-calibrating SAM data on dense clusters were presented by J. Sánchez at the conference Astrophysics at high angular resolution 2011 on 30 Aug 2011, in Bad Honnef, Germany. Publication in preparation. 485.L-0122: 5 hours of service mode time (PI Schödel) to determine an astrometric flat field for the NACO S27 camera with milliarcsecond accuracy. Data received in August 2010, analysis in progress, but very di cult because the service mode data were taken under extremely fast seeing with extremely small isoplanatic angle. This means that precision photometry across the S27 FOV is complicated because of the low Strehl ratio and spatially highly variable PSF. P87: 087.B-0658: 4h of service mode time on NACO (PI Schödel) for speckle holography of the Galactic center. Data acquired in August 2011. High-quality, high-strehl images were reconstructed from the data. Paper in preparation. 10a. ESO Archive - Are the data requested by this proposal in the ESO Archive (http://archive.eso.org)? If so, explain the need for new data. The requested data are NOT on the ESO Archive. Important. If data exist, then explain celarly why you need new data. 10b. GTO/Public Survey Duplications: 11. Applicant s publications related to the subject of this application during the last 2 years García-Marín, M.; Eckart, A.; Weiss, A.; Witzel, G.; Bremer, M.; Zamaninasab, M.; Morris, M. R.; Schödel, R. et al. 2011, ApJ, 738, article id.158: Extended Submillimeter Emission of the Galactic Center and Nearinfrared/submillimeter Variability of Its Supermassive Black Hole R. Schödel, M. R. Morris, K. Muzic, A. Alberdi, L. Meyer, A. Eckart & D. Y. Gezari 2011, A&A, 537, id.a83: The mean infrared emission of Sagittarius A* Girard J. H., Kasper M., Quanz S. P., Kenworthy M. A., Rengaswamy S., Schödel R. et al., 2010, Proceedings of the SPIE, 7736, 77362N: Status and new operation modes of the versatile VLT/NaCo Muzic K., Eckart A., Schoedel R., Buchholz R., Zamaninasab M., 2010, A&A, 521, A13: Cometary shaped sources at the Galactic Center - Evidence for a wind from the central 0.2 pc Schödel R., 2010, A&A, 509, A26: Accurate photometry with adaptive optics in the presence of anisoplanatic e ects with a sparsely sampled PSF. The Galactic center as an example of a challenging target for accurate AO photometry Schoedel R., Najarro F., Muzic K., Eckart A., 2010, A&A, 511, A18: Peering through the veil: near-infrared photometry and extinction for the Galactic nuclear star cluster. Accurate near infrared H, Ks, and L photometry and the near-infrared extinction-law toward the central parsec of the Galaxy Schödel R., Merritt D. & Eckart A., 2009, A& A, 503, 91-111: The nuclear star cluster of the Milky Way: proper motions and mass

10. Report on the use of ESO facilities during the last 2 years P85: 085.D-0214: 2 nights of visitor mode time at NACO (PI Schödel) for sparse aperture masking (SAM) interferometry on selected targets in the Galactic center, scheduled for 1-5 June 2010. Weather loss 50%, 20% low data quality because of extremely short atmospheric coherence time and low AO performance. 30% acceptable to good data quality. Analysis under way as part of PhD project of J. Sánchez. Preliminary results and a new way of auto-calibrating SAM data on dense clusters were presented by J. Sánchez at the conference Astrophysics at high angular resolution 2011 on 30 Aug 2011, in Bad Honnef, Germany. Publication in preparation. 485.L-0122: 5 hours of service mode time (PI Schödel) to determine an astrometric flat field for the NACO S27 camera with milliarcsecond accuracy. Data received in August 2010, analysis in progress, but very di cult because the service mode data were taken under extremely fast seeing with extremely small isoplanatic angle. This means that precision photometry across the S27 FOV is complicated because of the low Strehl ratio and spatially highly variable PSF. P87: 087.B-0658: 4h of service mode time on NACO (PI Schödel) for speckle holography of the Galactic center. Data acquired in August 2011. High-quality, high-strehl images were reconstructed from the data. Paper in preparation. 10a. ESO Archive - Are the data requested by this proposal in the ESO Archive (http://archive.eso.org)? If so, explain the need for new data. The requested data are NOT on the ESO Archive. 10b. GTO/Public Survey Duplications: Important. But hardly ever needed. 11. Applicant s publications related to the subject of this application during the last 2 years García-Marín, M.; Eckart, A.; Weiss, A.; Witzel, G.; Bremer, M.; Zamaninasab, M.; Morris, M. R.; Schödel, R. et al. 2011, ApJ, 738, article id.158: Extended Submillimeter Emission of the Galactic Center and Nearinfrared/submillimeter Variability of Its Supermassive Black Hole R. Schödel, M. R. Morris, K. Muzic, A. Alberdi, L. Meyer, A. Eckart & D. Y. Gezari 2011, A&A, 537, id.a83: The mean infrared emission of Sagittarius A* Girard J. H., Kasper M., Quanz S. P., Kenworthy M. A., Rengaswamy S., Schödel R. et al., 2010, Proceedings of the SPIE, 7736, 77362N: Status and new operation modes of the versatile VLT/NaCo Muzic K., Eckart A., Schoedel R., Buchholz R., Zamaninasab M., 2010, A&A, 521, A13: Cometary shaped sources at the Galactic Center - Evidence for a wind from the central 0.2 pc Schödel R., 2010, A&A, 509, A26: Accurate photometry with adaptive optics in the presence of anisoplanatic e ects with a sparsely sampled PSF. The Galactic center as an example of a challenging target for accurate AO photometry Schoedel R., Najarro F., Muzic K., Eckart A., 2010, A&A, 511, A18: Peering through the veil: near-infrared photometry and extinction for the Galactic nuclear star cluster. Accurate near infrared H, Ks, and L photometry and the near-infrared extinction-law toward the central parsec of the Galaxy Schödel R., Merritt D. & Eckart A., 2009, A& A, 503, 91-111: The nuclear star cluster of the Milky Way: proper motions and mass

10. Report on the use of ESO facilities during the last 2 years P85: 085.D-0214: 2 nights of visitor mode time at NACO (PI Schödel) for sparse aperture masking (SAM) interferometry on selected targets in the Galactic center, scheduled for 1-5 June 2010. Weather loss 50%, 20% low data quality because of extremely short atmospheric coherence time and low AO performance. 30% acceptable to good data quality. Analysis under way as part of PhD project of J. Sánchez. Preliminary results and a new way of auto-calibrating SAM data on dense clusters were presented by J. Sánchez at the conference Astrophysics at high angular resolution 2011 on 30 Aug 2011, in Bad Honnef, Germany. Publication in preparation. 485.L-0122: 5 hours of service mode time (PI Schödel) to determine an astrometric flat field for the NACO S27 camera with milliarcsecond accuracy. Data received in August 2010, analysis in progress, but very di cult because the service mode data were taken under extremely fast seeing with extremely small isoplanatic angle. This means that precision photometry across the S27 FOV is complicated because of the low Strehl ratio and spatially highly variable PSF. P87: 087.B-0658: 4h of service mode time on NACO (PI Schödel) for speckle holography of the Galactic center. Data acquired in August 2011. High-quality, high-strehl images were reconstructed from the data. Paper in preparation. 10a. ESO Archive - Are the data requested by this proposal in the ESO Archive (http://archive.eso.org)? If so, explain the need for new data. The requested data are NOT on the ESO Archive. 10b. GTO/Public Survey Duplications: 11. Applicant s publications related to the subject of this application during the last 2 years García-Marín, M.; Eckart, A.; Weiss, A.; Witzel, G.; Bremer, M.; Zamaninasab, M.; Morris, M. R.; Schödel, R. et al. 2011, ApJ, 738, article id.158: Extended Submillimeter Emission of the Galactic Center and Nearinfrared/submillimeter Variability of Its Supermassive Black Hole R. Schödel, M. R. Morris, K. Muzic, A. Alberdi, L. Meyer, A. Eckart & D. Y. Gezari 2011, A&A, 537, id.a83: The mean infrared emission of Sagittarius A* Girard J. H., Kasper M., Quanz S. P., Kenworthy M. A., Rengaswamy S., Schödel R. et al., 2010, Proceedings of the SPIE, 7736, 77362N: Status and new operation modes of the versatile VLT/NaCo Muzic K., Eckart A., Schoedel R., Buchholz R., Zamaninasab M., 2010, A&A, 521, A13: Cometary shaped sources at the Galactic Center - Evidence for a wind from the central 0.2 pc Schödel R., 2010, A&A, 509, A26: Accurate photometry with adaptive optics in the presence of anisoplanatic e ects with a sparsely sampled PSF. The Galactic center as an example of a challenging target for accurate AO photometry Schoedel R., Najarro F., Muzic K., Eckart A., 2010, A&A, 511, A18: Peering through the veil: near-infrared photometry and extinction for the Galactic nuclear star cluster. Accurate near infrared H, Ks, and L photometry and the near-infrared extinction-law toward the central parsec of the Galaxy Schödel R., Merritt D. & Eckart A., 2009, A& A, 503, 91-111: The nuclear star cluster of the Milky Way: proper motions and mass Hardly relevant. Good if recent publications exist, but has usually little influence on evaluation.

Hardly relevant for evaluation by panel, but make sure that your target list is complete (except ToO) and avoid any errors.

Hardly relevant for evaluation by panel, but make sure that your target list is complete (except ToO) and avoid any errors. Hardly relevant for evaluation by panel, but may be important for your observations.

Hardly relevant for evaluation by panel, but make sure that your target list is complete (except ToO) and avoid any errors. Hardly relevant for evaluation by panel, but may be important for your observations. Hardly relevant for evaluation by panel, but very important for your observations. In visitor mode you will ONLY be allowed to use requested modes.

Thank you.