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

Transcription

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

2 General Information

3 Video streams 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 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.

4 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 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.

5 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 Applicants will be informed about the outcome of the selection process as soon as possible after the deadline. ESO Electronic Newsletter, Dec. 2012

6 Upcoming instruments

7 Upcoming instruments MUSE - in 2013

8 Upcoming instruments

9 Upcoming instruments KMOS - commissioning ongoing

10 Evaluation Procedure

11 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)

12 Evaluation Criteria

13 Evaluation Criteria Be especially careful with re-submissions.

14 Grades

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

16 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.

17

18 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

19 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

20 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

21 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)

22 Keep in Mind Each referee has to read proposals (including ~10 large proposals). Typically 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.

23 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).

24 Proposal Form

25 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 Garching bei München opo@eso.org Tel. : 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

26 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 Garching bei München opo@eso.org Tel. : 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

27 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 Garching bei München opo@eso.org Tel. : 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

28 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 Garching bei München opo@eso.org Tel. : 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

29 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 Garching bei München opo@eso.org Tel. : 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

30 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 Garching bei München opo@eso.org Tel. : 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

31 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 Garching bei München opo@eso.org Tel. : 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

32 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 Garching bei München opo@eso.org Tel. : 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

33 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 Garching bei München opo@eso.org Tel. : 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

34 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 Garching bei München opo@eso.org Tel. : 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

35 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 Garching bei München opo@eso.org Tel. : 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

36 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 Garching bei München opo@eso.org Tel. : 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

37 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 Garching bei München opo@eso.org Tel. : 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

38 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 Garching bei München opo@eso.org Tel. : 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

39 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 Garching bei München opo@eso.org Tel. : 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

40 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 Garching bei München opo@eso.org Tel. : 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

41 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 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 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 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 ( ) 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, Lo & Claussen 1983, Nature, 306, 647. Lutz+ 1993, ApJ, 418, 244. Muzic+ 2007, A&A, 469, Paumard+ 2004, A&A, 426, 81. Schödel+ 2007, A&A, 462, L1-L4. Viehmann+ 2006, ApJ, 642, Yusef-Zadeh & Wardle 1993, ApJ, 405, 584. Zhao, Morris+ 2009, ApJ, 699,