- About this Journal ·
- Abstracting and Indexing ·
- Aims and Scope ·
- Article Processing Charges ·
- Author Guidelines ·
- Bibliographic Information ·
- Citations to this Journal ·
- Contact Information ·
- Editorial Board ·
- Editorial Workflow ·
- Free eTOC Alerts ·
- Publication Ethics ·
- Recently Accepted Articles ·
- Reviewers Acknowledgment ·
- Submit a Manuscript ·
- Subscription Information ·
- Table of Contents
Advances in Astronomy
Volume 2010 (2010), Article ID 253675, 7 pages
REM: Automatic for the People
1INAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, Italy
2INAF-Telescopio Nazionale Galileo, Rambla José Ana Fernández Pérez, 7 38712 Breña Baja, Spain
3INAF-Osservatorio Astronomico di Roma, Via di Frascati, 33 00040 Monte Porzio Catone, Italy
4INAF-IASF Bologna, Via Gobetti 101, 40129 Bologna, Italy
5Observatori Astronòmic de la Universitat de València, Edifici Instituts d'Investigació, Polígon La Coma, 46980 Paterna, València, Spain
6Dipartimento di Fisica, Facoltà di Scienze MM. FF. NN., Università degli Studi di Perugia, Via A. Pascoli, 06123 Perugia, Italy
Received 16 June 2009; Revised 27 November 2009; Accepted 18 December 2009
Academic Editor: Alberto J. Castro-Tirado
Copyright © 2010 Emilio Molinari et al. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
We present the result of a year-long effort to think, design, build, realize, and manage the robotic, autonomous REM observatory, placed since June 2003 on the cerro La Silla, ESO Chile. The various aspects of the management and control are here surveyed, with the nice ideas and the wrong dead ends we encountered under way. Now REM is offered to the international astronomical community, a real, schedulable telescope, automatic for the People.
1. Half a World Away
REM (Rapid Eye Mount) was thought and realized in order to catch fast optical and infrared transient phenomena, correlated with high-energy events signaled by orbiting observatories, mainly GRB discovered by then recently launched Swift satellite. Its realization resulted in a workbench for various other existing and wish-list telescopes [1–3] (see also http://www.rem.inaf.it/).
The statistics of pre-Swift bright GRB optical transient led to a 60 cm diameter telescope, equipped with VIS/IR cameras, fast enough to follow Swift acrobatics and to acquire images, process them fast, and detect the transient with good accuracy to alert larger telescopes’ spectrographs. We decided, in order to put it far from existing or proposed robotic telescopes, half a world apart in the southern hemisphere, on the Chilean Andes in the ESO site of La Silla.
2. Losing My Religion
In order to fulfill the requirements the telescope should have had the capabilities to react immediately to alerts, see the afterglow of the GRBs, and classify it to estimate the redshift by photometry. To this extent the mechanics of the telescope should have been robust and fast enough, the size of the mirror should have been large enough, and the photometry was needed in both visible and infrared. On the software side we should be able to control the telescope, command both cameras and analyze the images, and at the end also alert the rest of the world. Were we good at this? Unfortunately the belief that GRB afterglows were bright enough for our chosen size of 60 cm as primary mirror revealed false, and the mean, dim luminosity of the transients de facto prevented REM, as most of the other robotic telescopes of the same class, to observe a large fraction of the afterglows following Swift satellite alerts. In those early times, before we could enhance the REM pointing capabilities to observe down to 5 degrees above horizon, only 5% of the GRB alerts could be reached by REM pointing. Our lack of ability to detect precise coordinates in due time also led to abandon the finalization of the transient detection and alert software, which remained at the still remarkable level of producing automatic astrophotometry for good quality images.
The robotic nature also revealed to be somewhat tricky and we had to add to our system a full self-telemetry of vital signal of the various subsystems which was also able to send SMS and e-mail to real people. A team of trained real people on-site was also required and we received the help and collaboration from ESO-La Silla technical staff, which is now able to intervene in case of need or emergency.
After we added the funded possibility to use REM as a laboratory for new technologies and finally offered the nonalert time to the astronomical community via the classical systems of call for proposals, we finally completed the REM Observatory, working regularly and autonomously every night since 4 semesters (a full photo in Figure 1).
3. All the Right Friends
The companies and developers involved in the REM realization were both from the private industry and from public research institutions. Halfmann Teleskoptechnik designed together with our group the telescope body and main reflecting Zeiss optics, coated by Sagem with protected silver to enhance the performances in the infrared. The main near infrared REMIR camera [4, 5] was designed by the gOlem group of the Brera Astronomical Observatory and assembled in the US-based Infrared Lab. An engineering Hawaii I chip from Rockwell was used in its best quadrant, with 512 512 pixels on a 10 10 arcmin field of view. The visible camera and spectrograph ROSS , also designed by gOlem, hosts SILO optics in a mechanical assembly manufactured by Perugia University and Brera Observatory workshops. The same field of view of REMIR is imaged by means of Zaot coated dichroic with a 1 m cut on a 1 K 1 K ALTA camera by Apogee. In Figure 2 the same field of view is observed with both cameras.
The REM dome is positioned in the ESO La Silla premises and can profit of all the (still, at date of writing) existing infrastructures and facilities. ESO provides power, UPS, and network connections, as well as liquid nitrogen refilling every 4 days. In every assembling phase the availability of a mechanical workshop and a clean room for the infrared detector assistance proved to be essential and both time sparing and mission proved to be critical.
The dome realization was performed by ESO general services and has two sliding roof which leave completely clear the sky without the need to have any movement during the observations (see a CAD rendering in Figure 3). Notre Dome opens when the Sun is below the horizon and all the safety parameters are within the limits; otherwise the telescope room is air conditioned and telescope parked in home position. The temperature inside the dome follows nervertheless the day/night cycle and a better thermal insulation would be required. The inner relative humidity never hits the excess of outer values and no dew point conditions were so far recorded. We finally rely on ESO and local meteo measurements to define safety conditions. Humidity below 90%, wind speed lower than 17 m/s, external temperature above C, and Sun below horizon are the main safety parameters, although a check on the open status of other domes in the La Silla site revealed to be a good choice, so that we will perform normal operations only when two other telescopes are observing.
5. Imitation of Life
The way REM acts is badly an imitation of autonomous machine. It needs a daily check from Italy in order to catch in with its many unforeseen situations and also, although now rare, unrecoverable stops in its sequences of jobs. In fact, we experienced some dome blockings, few main computer crashes and network halts, as well as some CCD driver timeouts. Many of these we recovered by remote commands but in some cases we had to wait for human help in La Silla.
Nevertheless its main sign of activity is the reaction to inputs. The main information flux starts from the Observing Block Scheduler which enters in the REM Observing Software (REM-OS, cfr. Stefanon et al. in this volume ) the sequence of targets, which is reorganized should a GRB alert or other boundary conditions occur (e.g., high airmass due to delayed observations). The flux eventually ends delivering a series of outputs: the raw data and processed photometric catalogues are immediately sent to the Bologna REM database, where PIs can retrieve their data and the general public can browse the complete observing log and retrieve all calibrations and standard stars. In the meantime a continuous cross-talk between REM-OS and the in situ internal telemetry database as well as the controls of telescope and cameras allow the images to be acquired safely.
A series of (mainly) python programs run autonomously in the various machines in the dome to get the status of the sensors, encoders, and so forth, and fill the proper SQL tables in the REM-OS machine.
The control python program is the tREM-o-meter which runs every 2 minutes. The tREMometer collects the relevant data from archive, fills in the missing values, produces a public web page with the status of the telescope and all subsystems and performed observations, and, finally, checks for malfunctions and sends e-mail and SMS alerts. In case the conditions become dangerous in the infrared Dewar (the most delicate area), it is able to autonomously interrupt all IR data acquisitions. We in fact allow a small range in IR chip temperature as safe operational range: should the sensor get heated more than 105 K, the IR camera is turned off, returning to normal operations only after its temperature is lower than 100 K.
6. Until the Day Is Done
Figure 4 at a glance gives to the human control people the instant situation of the alarm status (checking temperature and pressure in the infrared Dewar and also the telescope control hardware for failure to respond to Remos command) and the job REM is actually performing in the night. The scheduled targets are listed in the sequence they will be observed. Such schedule is continuously recomputed after every observation because the optimal conditions for the next target may be affected by some misbehavior during the last acquisition (delays, repeated frames, etc.). When the night is done, all blue dots will disappear and soon a new schedule for the next day is arranged. After every observing night every PI involved in recent observations is noticed by an automatic e-mail from the REM archive.
The monitoring of the dome opening together with shutter-open time of every acquired image is the content of Figure 5. The La Silla domes monitoring proved essential to the security of the REM operations, as we ended opening the dome only when our meteo station gives good measures, as well as the ESO one, and two other domes are open in the site. We are thus able to produce independent meteo statistics for the ESO La Silla site as well as our own efficiency rate (Figure 6).
Other plots in the tREMometer include the status of the cryostat, temperatures, and meteo data from REM meteo station. Also, the program offers a Gannt graph of the past night, allowing the REM team to check for inconsistencies in the programmed observations. The degraded, small image previews are then posted on the web site for PI and public access.
During the following morning, every PI whose observations were continued in the previous night receives a detailed e-mail directly from the database in Bologna.
Furthermore, the Remos machine produces weekly reports which are sent to a restricted set of people: first, a report on a 4-month timeline of the pressure in the REMIR Dewar and the daily consumption of the liquid nitrogen supply. These are very useful to program mid term maintenance, such as repumping the vacuum in the cryostat and in the nitrogen lines.
The last information sent by the Remos system is the status of the observing programs accepted by the Italian Time Allocation Committee, allowing to follow the completion of the requested observations. In the last completed call (AOT18) all programs were well above 80%, not counting the ToO which did not use all their time.
7. 1 000 000
The final repository for all the REM images is the REM Archive in Bologna. After an image is written on disk in Chile by the cameras, it is processed for quick astrophotometry and then sent to the database together with other data. In May 2009 the number of entries in the archive overcame 1 000 000. The archive web browser allows identified users to use a password layer to access their private data as well as all the public calibration frames.
Various preset types of query can be used to select and then retrieve the wanted images, and as well a custom SQL WHERE clause may be entered by the user.
It is also possible to perform basic on-line analysis on the observations, grouping by date or type, and showing the object position on the sky as shown in Figure 7.
Among the 1 million images many have found their place in high ranked scientific papers, both in GRB science  and in other topics such as blazars . In fact, even if GRBs are fainter than thought, the fast reaction time of REM allowed us to observe the onset of the infrared afterglow, leading to the measure of the expansion velocity of the fireball. The mean elapsed time for REM observing after a satellite alert is 30 seconds as shown in  and the time resolution can be as fast as 1 second when the afterglow is bright enough.
8. Everybody Hurts
Even the most exciting project comes to a regime cycle that can hurt the creativity of a research group. REM Team to avoid becoming a managing and maintenance unit for yet another telescope turned the REM observatory into a working laboratory for experimenting new devices.
The first was the change in cooling system for the REMIR camera. The on-board Stirling cryocooler by Leibold Vacuum presented a series of problems ending in a serious instability of the system. The main problem was the underdimensioned power for our heat removal needs, but the Leibold company itself admitted that the maintenance of such cryocooler was so difficult that at the end they dismissed the production. Thus we adopted an ad hoc modified Continuous Flow Cryostat, a cryogenics system developed by ESO and extensively used in ESO instrumentation, whose main characteristic is that the LN2 vessel is separated from the cryostat, allowing a greater LN2 tank, then really improving the hold time . We are now able to run continuously the telescope with one LN2 tank change every 4/5 days. In normal conditions this is the only human intervention REM needs to work.
A completely new experiment was also conceived in collaboration with IASF-Bologna, University of Bologna and SAO (Russia). TORTORA [11, 12] is a separated telescope hosted in parallel to REM, mechanically fixed in the same mount (see Figure 1). The aim was to study short stochastic optical flares of different objects (GRBs, SNs, etc.) of unknown localization. To this purpose it is necessary to monitor large regions of sky with high time resolution and we developed a wide-field camera (FOW is 400–600 sq.deg.) using TV-CCD with time resolution of 0.13 second to record and classify optical transients. The photometer can reach mag 10.5 in one single 0.13 second exposure. Together with REM cameras it forms the telescope complex TORTOREM, operated from May 2006 by the joint teams of REM and SAO. The main result was the serendipitous observation of GRB080319B, a naked-eye burst whose light curve could be monitored in high time frequencies  as reported in Figure 8.
The future step of the REM lab will be the complete replacement of the optical camera ROSS. ROSS2 will have better optical quality which revealed not being optimized in the present camera and will produce 4 simultaneous images in the Sloan passbands , , , and . Figure 9 sketches the optical design which makes heavy use of dichroics.
9. The Great Beyond
The experience of this project will not be lost. Our team is now deeply involved in the conceptual design of a 4-meter class telescope which will have a simultaneous camera like ROSS2 which extends into the infrared up to band. Its response time after alerts will be comparable with REMs, aiming to the target within well under one minute . Its capabilities will be coupled with a battery of wide field, fast photometer telescopes which in principle should cover the whole sky or a great portion of it and be able to generate alerts instead of reacting to satellites.
The authors acknowledge the effort from all people which made REM possible; in particular the four ESO musqueteers in La Silla which helped and collaborated with them since the beginning and without their skill the project could have been in serious troubles. Also, they thank the American rock band R.E.M. for their prophetic song titles which have been used in this article.
- F. M. Zerbi, G. Chincarini, G. Ghisellini, et al., “The REM telescope, a robotic multiwavelength facility,” in Ground-Based Instrumentation for Astronomy, A. F. M. Moorwood and M. Iye, Eds., vol. 5492 of Proceedings of SPIE, pp. 1590–1601, Glasgow, UK, June 2004.
- G. Chincarini, F. Zerbi, A. Antonelli, et al., “The last born at La Silla: REM, The Rapid Eye Mount,” The Messenger, vol. 113, pp. 40–44, 2003.
- S. Covino, M. Stefanon, G. Sciuto, et al., “REM: a fully robotic telescope for GRB observations,” in Ground-Based Instrumentation for Astronomy, A. F. M. Moorwood and M. Iye, Eds., vol. 5492 of Proceedings of SPIE, pp. 1613–1622, Glasgow, UK, June 2004.
- P. Conconi, R. Cunniffe, F. D'Alessio, et al., “The commissioning of the REM-IR camera at La Silla,” in Ground-Based Instrumentation for Astronomy, A. F. M. Moorwood and M. Iye, Eds., vol. 5492 of Proceedings of SPIE, pp. 1602–1612, Glasgow, UK, June 2004.
- F. Vitali, F. M. Zerbi, G. Chincarini, et al., “The REM-IR camera: high quality near infrared imaging with a small robotic telescope,” in Instrument Design and Performance for Optical/Infrared Ground-Based Telescopes, M. Iye and A. F. M. Moorwood, Eds., vol. 4841 of Proceedings of SPIE, pp. 627–638, August 2002.
- G. Tosti, M. Bagaglia, C. Campeggi, et al., “The REM optical slitless spectrograph (ROSS),” in Ground-Based Instrumentation for Astronomy, A. F. M. Moorwood and M. Iye, Eds., vol. 5492 of Proceedings of SPIE, pp. 689–700, Glasgow, UK, June 2004.
- M. Stefanon, et al., “The REM observing software,” accepted in Advances in Astronomy.
- E. Molinari, S. D. Vergani, D. Malesani, et al., “REM observations of GRB060418 and GRB060607A: the onset of the afterglow and the initial fireball Lorentz factor determination,” Astronomy & Astrophysics, vol. 469, no. 1, pp. L13–L16, 2007.
- A. Giuliani, F. D'Arrimando, S. Vercellone, et al., “AGILE observation of a gamma-ray flare from the blazar 3C 279,” Astronomy and Astrophysics, vol. 494, no. 2, pp. 509–513, 2009.
- F. Vitali, J. L. Lizon, G. Ihle, et al., “The REMIR cryogenics restyling,” in Ground-Based and Airborne Instrumentation for Astronomy, I. S. McLean and M. Iye, Eds., vol. 6269 of Proceedings of SPIE, Orlando, Fla, USA, May 2006, 626954.
- S. Karpov, et al., “Wide and fast monitoring the sky in subsec domain,” accepted in Advances in Astronomy.
- E. Molinari, G. Beskin, S. Bondar, et al., “Ground-based complex for detection and investigation of fast optical transients in wide field,” in Ground-Based and Airborne Telescopes II, L. M. Stepp and R. Gilmozzi, Eds., vol. 7012 of Proceedings of SPIE, Marseille, France, June 2008, 70122S.
- J. L. Racusin, S. V. Karpov, M. Sokolowski, et al., “Broadband observations of the naked-eye -ray burst GRB 080319B,” Nature, vol. 455, no. 2008, pp. 183–188, 2008.
- F. Vitali, et al., “A path to the stars: the evolution of the species,” accepted in Advances in Astronomy.