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Project STELES – SOAR Telescope Echelle Spectrograph For technical details see: www.lna.br/~stelles

INDEX

Abstract………………………………………………………………………………………2 1- Scientific Drivers 1.1 Introduction……………………………………………………………………………..3 1.2 Research fields that will benefit from STELES data…………………………….4 1.3 Access to the Instrument…………………………………………………………….7 1.4 Expected results……………………………………………………………………….7 2- Results transference methodology.……………..…………………………………..7 3- Project Methodology 3.1 Technical viability……………………………………………………………….…..…8 3.2 Instrument operation……………………………………………………….………….8 3.3 Maintenance plan………………………………………………………………………8 4- Management Approach 4.1 Construction……………………………………………………………………………9 4.2 Technical management……………………………………………………………….9 4.3 Follow up and documentation………………………………………………………9 4.4 Financial management………………………………………………………………10 4.5 Risk analysis………………………………………………………….……………….10 4.6 LNA infrastructure for production and assembling STELES………….……..11 5 Personnel 5.1 The instrument team and participants in the project……………………….…11 5.1 Potential users…………………………………………………………………….....12 6- Budget…………………………………………………………………………………..15 7- Simplified Schedule – indicating principal stages and estimate times……..16 8- Outreach………………………………………………………………………….…..…16 9- Bibliography 9.1 Technical publications……………………………………………………….……..16 9.2 Sample of science papers……………………………………………………....….17

Appendix A Equipment to be purchased in Brazil………………………………………...……….19 Equipment to be imported……………………………………………………………….19 Supplies and items to be purchased in Brazil…………………………….…..…….19 Supplies and items to be imported…………………………………………………....20 Third part labor in Brazil…………………………………………………………………22 Third part labor to be contracted outside Brazil………………………………....…22 Travel expenses…………………………………………………………….………..…...24 Daily expenses…………………………………………………………….…….…….….24 AppendixB Letter from SOAR Director approving STELES as a second generation instrument………………………..………………………….…………………….…....…24

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ABSTRACT High resolution spectroscopy has had an enormous scientific value for Brazilian

astronomers, however, up to now we have not had access to an efficient instrument in a telescope with enough number of nights such as the 4.1 meter SOAR. For that purpose we intend to build the optical and mechanical modules of the STELES spectrograph, which the Brazilian community is committed to offer to the SOAR consortium. We developed a design with higher, wider spectral response and at lower cost throughput than instruments of the same class currently in operation. The project is already approved by the SOAR Board of Directors, 1/3 of the parts have been already purchased, and we plan to commission the instrument before 2010. The complex and diverse technologies of the instrument, such as fine mechanics, optics, electronics, cryogenics and software are interesting for the development of the national industry. In addition to burst the productivity of the Brazilian Astronomy, the instrument will have significant international visibility, since it will also be used by our partners from the USA and Chile.

Layout of STELES spectrograph, showing the red and the blue arms

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1- Scientific Drivers

1.1 Introduction High-resolution spectroscopy (HIRES) is one of the most powerful astronomical techniques.

It enables determination of physical parameters such as temperature, gravity, rotation, radial motion and chemical composition. Abundances can be derived for stars in the Milky Way, in nearby galaxies and also in distant protogalactic clouds projected in the line-of-sight of quasars, probing the local and high-redshift Universe. Comparison between near and far universe gives information about its evolutionary phases, such as the first stellar generation, the epoch of re-ionization, and the formation of the galaxies.

The Brazilian astronomical community has intensively been using high-resolution spectroscopy. Before the 1990’s, the access to this technique was provided mainly through foreign facilities: ESO (European Southern Observatory) and CTIO (Cerro Tololo Interamerican Observatory), but after that, only projects in collaboration with researchers from the host institutions were possible, narrowing the access to the Brazilian community. In the period 1998-2002, under an agreement between ESO and ON (Observatório Nacional), Brazil rented the 1.5-m telescope at La Silla, enabling many projects to be developed. Currently, the access to HIRES instruments are through bHROS (optical range) and PHOENIX (near infrared) on Gemini South, but it is limited to a few nights per year for the whole Brazilian community. Therefore, we need urgently a HIRES facility on SOAR, where we have ~100 nights/year. The STELES spectrograph (www.lna.br/~stelles) will reach objects as faint as V=18 (S/N=10 in one hour) with a spectral resolution R=50000, enabling science observations of objects hundreds of times fainter than what can currently be done in the main Brazilian facility, the Observatório Pico dos Dias (OPD). A set of projects that will take advantage of the proposed instrument is presented below.

The construction of STELES (SOAR Telescope Échelle Spectrograph) is already approved by the SOAR project as a second generation instrument, such that our community is committed to deliver it on time. STELES will be part of the set of instruments of the SOAR telescope, built by an international consortium between Brazil(CNPq), USA(NOAO, Michigan State University, University of North Carolina) and Chile(Conicyt). The expected high quality data are prone to produce important scientific results for us and the whole SOAR partnership, resulting in a good visibility to our technical capability. The development of a world-class instrument is also important to acquire a forefront instrumental knowledge.

The layout of STELES was developed in the period 2001-2006, as part of the Instituto do Milênio para Evolução de Estrelas e Galáxias na Era dos Grandes Telescópios: implementação de Instrumentação para os Telescópios SOAR e Gemini leaded by Beatriz Barbuy (IAG-USP). The layout is already reviewed and approved by the SOAR consortium. After that, the Millennium Institute bought the CCD arrays for the blue and the red arm, the controller and the cryogenic dewars, amounting to 1/3 of the total cost of the project.

Building instrumentation for a 4-m class telescope requires complex technologies involving engineering skills on fine mechanics, electronics, software, cryogenics and optics. All the different parts are developed simultaneously, around the core that is the optical design. The present project is concerned about the optics and mechanics of the instrument.

The Optical concept of STELES was designed by Bernard Delabre from ESO, one of the most prestigious optical engineers specialized in astronomical instrumentation. The project was conceived in an intense collaboration with Bruno Castilho and Clemens Gneiding from LNA/MCT. New achievements resulted in an instrument that is more efficient, cheaper and with higher throughput than similar instruments at work, such as FEROS, for example.

The optics of this kind of instrument cannot be ordered from commercial factories, but instead it has to be designed individually to achieve optimal performance. It is divided in 4 basic

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modular parts: a) the blue camera, b) the red camera, c) the fore-optics and d) the intermediate lenses and collimators. The mechanics is split into the fore-optics and the optical bench where the optical elements are mounted. In this project submitted to FAPESP we plan to buy the optical and mechanical parts and assemble the instrument. As in the previous phases of this instrument, the tight collaboration between IAG/USP and LNA/MCT is crucial for its successful completion. LNA infrastructure in optical metrology and characterization will be used to test and evaluate the optical components and verify if they are within the project specifications. LNA will be in charge of the optical assembly and alignment procedures, and the tools for these tasks are already purchased under FINEP and LNA projects.

1.2 Research fields that will benefit from STELES data HIRES has a great impact in all fields of Astrophysics. STELES will combine high spectral

resolution (6 Km/s/pixel), high stability, broad wavelength coverage (300-1000 nm), and good performance in the UV, and a fast, optimized data reduction software. Many existing projects in the Brazilian community will benefit from these capabilities and opportunities will be opened for new projects, which are currently impossible to be conducted. We list below a sample of such projects. Please notice that the references are intended to exemplify what the Brazilian community is doing, and so, is not exhaustive in any sense. Other papers from the same authors can be found in the web.

a- Abundance analyses in the near-UV: Key projects requiring good efficiency in the near-UV include spectroscopy of the strong electronic OH lines near 3100Å. These particular OH lines are detectable to very low metallicity and are useful in attempts to derive oxygen abundances in the oldest stars in the Galaxy: such O abundances probe the very earliest chemical evolution in the Milky Way. In addition to OH, the element beryllium is only detectable in the near-UV, via Be II lines near 3130Å. Beryllium is produced only through cosmic-ray spallation reactions and is a key probe in understanding cosmic-ray nucleosynthesis over the chemical evolutionary history of the Galaxy (Castilho et L. 1999, Cayrel et al. 2001).

b- Chemical Evolution of the Galaxy: The chemical evolution of the Galaxy follows the changes in elemental abundances from their initial values into the present compositions of the disk, bulge and halo. Some examples of specific topics related to this subject are the gradients of metallicity (Daflon and Cunha 2004) and radial and temporal variations of the star formation rate (Rocha-Pinto et al. 2000, Maciel et al. 2006). Also, detailed chemical composition analyses reveal measurable heterogeneities, possibly associated with age and position in the Galaxy, suggesting that local enrichment events may play a role in the overall galactic metal production (Castro et al. 1999). Concerning the major components of the Galaxy, the study of the bulge is essential to understand the mechanisms of formation of our Galaxy: the bulge may have been formed in the beginning of our Galaxy, although part of the bulge may have formed significantly later. The study of the oldest halo stars provides crucial lithium abundances that result from primordial Big Bang nucleosynthesis. Young stars in the Galactic disk trace the present distribution of chemical abundances and can be used to determine abundance gradients: these gradients provide constraints to Galactic models of star formation and chemical evolution (Barbuy et al. 2003).

c- Stars enriched by the r- and s-process: It has been suggested that one likely explanation for the highly r-process enhanced stars that have been identified recently is that they are members of a binary system with a massive companion that exploded as a type II supernova, which would now be a collapsed object such as a black hole. By monitoring radial velocities of the many examples of these stars we hope to find in the near future will be of extreme importance. The same applies to the metal-deficient stars that are moderately enhanced in their r-process elements (Barklem et al. 2005, Rossi et al. 2005). Additionally, s-process enriched stars such as barium stars have a complicated pattern of overabundance of s-process elements that has defied any straightforward interpretation. The well accepted model of wind accretion establishes that a trend of overabundance with the binary system period should be observed, which is not corroborated by observations. Even the

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nuclear reaction responsible for neutron production is controversial, since the preferred 13C (alpha, neutron) 16O reaction predicts a trend of both the overall overabundance and the neutron exposure parameter with metallicity, again directly contradicting the observations (Smiljanic, Porto de Mello, da Silva, 2006 A&A, accepted). Detailed analysis of large samples of these objects, involving many elements, is the only way to provide the necessary observational constraints to clarify these issues.

d- Light Element Abundances: The primordial abundance of light elements and their subsequent Galactic enrichment requires high-quality data to constrain and test their production and evolutionary models. One important problem in this subject is the intrinsic dispersion of Li abundances in dwarf stars of halo globular clusters. Given that globular clusters are among the oldest objects in the Galaxy, their initial Li abundance must be very close to the primordial value. Precise abundance determinations for Li (both 6Li and 7Li) and Be (with only one stable isotope, 9Be) provide essential information relevant to early Galactic cosmic-ray fusion and spallation nucleosynthesis, as well as primordial Big Bang Nucleosynthesis. Beryllium is an important addition to lithium, but Be is much more difficult to observe. The spectral regions containing the Be II (3130.41Å and 3131.06Å) and Be I lines (3312Å) are crowded and close to the atmospheric cutoff: a near-UV optimized spectrograph, such as STELES, would be an important addition to light element studies.

e- Cluster Analyses: The determination of accurate abundances in globular cluster stars over a range of magnitudes, covering effective temperatures from 4000 to 6000 K, can address the issue of possible variations in chemical composition existing among stars belonging to the same cluster. This topic is particularly relevant in investigating possible stellar processes, such as diffusion, dredge-up (Barbuy et al. 2006, Alves-Brito et al. 2005). The chemical distribution in sparse young clusters can be studied in significant samples of OB stars in OB associations (Daflon, Cunha and Buttler 2004). STELES will be able to investigate stars down to the main-sequence turn-off (V=17) in several clusters, combining high efficiency with a wide spectral range. Superb image quality, will also allow for spectroscopy in relatively crowded cluster fields.

f- Long-Term Velocity Monitoring of Carbon-Enriched Metal-Poor stars: A large fraction of the stars with [Fe/H] < -2.5 exhibit anomalously strong CH G-bands (and often C2 and CN features) indicative of very high carbon abundance, despite the stars overall low metallicity. It seems quite unlikely that all of the stars involved are members of close binaries that have undergone mass transfer of carbon-enriched material from their companions. Hence, sorting out which of the stars are radial velocity variables and which are not is an important program. Since the periods of known mass-transfer binaries can reach up to 7-8 years (or more, in some cases), gathering data for their study is a challenge with most telescopes. Correlations between measured abundances of (e.g., s-process) elements and orbital properties would provide valuable clues for understanding the range of phenomena and the nature of the progenitors in these systems (Lucatello et al. 2006, Rossi et al. 2005).

g- Asteroseismology of stars: Some structural properties of stellar interiors can be probed by the study of the weak non-radial pulsations that have been observed in objects all over the HR diagram, requiring simultaneous measurement of many spectral lines leads to the detection of multiperiodic oscillations. A large fraction of high mass stars with envelopes display non-radial pulsations, indicating that this is a relevant ingredient for mass ejection, in addition to the classical stellar winds. Asteroseismology is an important tool for stellar evolution studies (Floquet et al. 2002, Levenhagen et al. 2003).

h- Stellar winds: mass loss affects significantly the lifetime of high mass stars. In late evolutionary phases, the wind can be so dense as to preclude direct assessment of the underlying photosphere. Fortunately, presently there are computing codes able to derive parameters for the wind and the photosphere in a coherent way. They are especially useful to interpret spectra of O-type stars, Wolf-Rayets, Luminous Blue Variables and central stars of planetary Nebulae, taken at

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high resolution and encompassing broad wavelength range (Steiner and Damineli 2004). Long-term monitoring is crucial to unveil the nature of evolved massive stars (Damineli 1996) and their mass loss rates. Most of the known objects of this type can be reached from the Southern Hemisphere.

i- Stellar rotation: All stars rotate at some level, but this parameter was included in the models only very recently. Predictions of luminosity, evolutionary tracks and times, chemical yelds are different from the case of non-rotating stars. There are still few observational tests for such models, but recently it was confirmed that the angular momentum migrates to the surface as the star approach the exhaustion of H in the core (Groh et al. 2006). This result has a strong impact on massive stars, since it affects the understanding of mass loss rate, bipolar flows and hypernovae explosion. The discovery was done with spectrographs similar to STELES. Studies on other fast B-type rotators have been done by (Vinicius et al. 2006) and the induced mixing has been tested for a sample of stars in the Galaxy and in the LMC (Daflon et al. 2001, Korn et al. 2005).

j- Young stars: Many parameters from Pre-Main Sequence (PMS) stars can be derived from HIRES, such as chromospheric activity (Vieira et al. 1999), Lithium abundance, rotation, binarity (Pogoding et al. 2006), magnetic fields (Pogodin et al. 2005) and cluster motion. Nearby young associations can indicate how the local Interstellar Medium evolved along the last 100 million years. On the other hand, that is the age at which we expect planets being formed around those stars. Determining the rotational velocity of those stars can give information about the evolution of rotation along the latest PMS phases and planetary formation (Torres et al. 2006). Abundances and mettalicities have been derived, based on spectral synthesis (G. Rojas, J. Gregorio-Hetem 2005), of young stars that are candidates to present debris disks (Gregorio-Hetem & Hetem 2002). One of our main interest is to characterize the stars which will be prime targets of NICI imaging as contribution from our team to the NICI planet campaign. Our projects are also related with the study of chemical abundance of the Galaxy and the analysis of stellar clusters.

k- Doppler tomography of accretion disks: Monitoring the variability of emission line profiles can be used to map discs and motion of circumstellar gas flows in binary systems with mass transfer. Although those systems, as seen from Earth, span only a few micro-arcsecond, their spatial structures can be resolved in detail with this technique (Diaz and Ribeiro 2003). The stochastic nature of the emission in lines can be analyzed by using large number of spectra with fine spectral and temporal sampling (Diaz 2001). This technique can be applied to many types of objects, like Cataclismic Variables with discs, Algol binaries, Classical T Tauri and Herbig Ae/Be.

l- Absolute dimension determination and spectral disentangling: the absolute dimensions of stars, mainly of masses and radii, but also effective temperatures, are the most important parameters in controlling the models for stellar formation, structure and evolution. The tendency of hierarchical clustering is revealing that more and more eclipsing binaries are in fact triples or quadruples (Casey et al. 1998). Many systems, especially the ones with young components, can only be analyzed through spectral disentangling techniques. As a by-product, the disentangled spectra are fully adequate for abundance studies. High-precision (S/N) and high-resolution spectroscopy are the desired qualities of the spectroscopic data for these tasks (Torres and Vaz 2006).

m- Post-AGB stars: Post-AGB stars are luminous objects of low and intermediate mass (M~8-9M ) in a final stage of evolution. They end their Asymptotic Giant Branch (AGB) evolution by a phase of very strong mass loss (10-7 - 10-4 M /yr), evolve on a fast track to hotter effective temperature at roughly constant luminosity but are not yet hot enough to ionize the cirumstellar material and to emerge as a planetary nebula prior to cool down as a white dwarf. The chemical composition of a post-AGB star should reflect the initial composition of the object, modulated by dredge-up process of nucleosynthetic ashes from the stellar interiors. The aim of this study is to determine the photospheric composition of post-AGB stars in order to constrain the chemical evolution as well to test the stellar evolution models of low and intermediate stars (Pereira and Roig 2006, Pereira et al. 2004).

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These are a few examples of projects being conducted by Brazilian astronomers, but many others, involving Novae, Supernovae, QSOs, AGNs will be feasible with STELES on SOAR.

1.3 Access to the instrument STELES is being built in Brazil in a collaboration between IAG, LNA and other Institutions

and will be available at SOAR telescope. The access to telescope time is proportional to the share of the partners: Brazil (31%- major partner), NOAO (30%), MSU (16%), UNC (15%) and Chile (10%). After being commissioned, the spectrograph is expected to be competitive along ~10 years, which can be extended by upgrades in technical parts (detectors, gratings, electronics) or reconfiguration to higher resolution to search for extrasolar planets, for example. When in operation all astronomers from Brazil (250 PhDs) and from the partner countries (USA and Chile) will be able to use it, by submitting proposals. In Brazil, such proposals are reviewed twice a year and ranked by a scientific committee nominated by the LNA CTC (Technical Scientific Committee) formed by members of main Brazilian Astronomical institutions meets twice a year. This follows a long tradition of peer revision in international science. The procedures of the Brazilian Time Allocation Committee for SOAR can be seen at: http://www.lna.br/soar/NSO/SOARNSO.html

The Brazilian community has been using intensively HIRES techniques. About 30% of the available time in the 1.6-m telescope at the OPD Observatory (http://www.lna.br) is allocated to high resolution spectroscopy. Based on the profile of our community an on that of our partners, and taking into account the other instruments available on SOAR, we predict that STELES will receive 15-20% of the load for telescope time.

1.4 Expected results STELES will definitely produce a strong impact in the Brazilian astronomy. We have

performed a forecast for the scientific production based on STELES data. This estimate is based on the historic usage of OPD and Gemini Observatories, and scaled for the size and number of spectroscopic nights on SOAR, adopting 10 years as the lifetime of the instrument. Those numbers may be underestimated, since the access to fainter targets and the optimized data reduction software will increase the productivity.

- PhD thesis: 15 - Master thesis: 15 - Postdocs fellows : 15 - Refereed papers: 175 - Papers in proceedings: 250 - Citations: 2000

2 – Results transference methodology Apart from the primary scientific results due STELES data, the STELES team is aware of

the amount of scientific and technological information which derives from the instrument development and construction, and we believe that this knowledge must be spread in order to support new developments in this and related areas.

A Metrology Laboratory in Optics has been constructed as part of a strategic plan of LNA to provide services for scientific and industrial needs from all over Brazil. Prototypes of components will be fabricated before the final construction in order to check if the specifications of the instrument will be achieved. In particular, an infrastructure for characterization of volume-phase-holographic gratings (VPH) and wide band anti-refection coatings is under construction at LNA.

The manual of the instrument, the control software and the reduction data package will be published in a specific Internet WebPage. In this way, users can use it efficiently and give feedback to the team to fine-tune the operational mode of the spectrograph. This will also help other groups

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developing instruments for SOAR to use the techniques included in STELES. A very detailed and easy to access manual is a fundamental feature in the context of the remote operations. The instrument at the telescope in Cerro Pachon will be operated from the six Remote Observing Stations in Brazil, the first one already in operation at IAG/USP. The computer codes will be based mostly on free access programming tools, in order to disseminate to other Institutes the techniques and standards used for instrumental control and data reduction.

3 – Project Methodology

3.1 Technical viability STELES is already approved by the SOAR Board of Directors, as a second generation

instrument, in order that its installation and operation is part of the Observatory plans. The development of STELES is supervised by the SOAR director, in order that all technical issues can be solved on time and following the SOAR agenda, avoiding conflicts with other planned instruments. SOAR has envisage a series of reviews during STELES development to guarantee the product quality and compliance with the project requirements.

Since STELES is a SOAR community project it will make use of existing SOAR facilities such as electric power, cryogenics (liquid nitrogen and cooling fluid in closed loop) and Internet access. In addition, it will use the calibration lamps, the guiding unit and the atmospheric refraction corrector, which demands small changes already in study by SOAR. These facilities are included in the SOAR budget. The transportation to Chile, installation at the telescope, commissioning and acceptance tests will be performed by the STELES team. This will take about three weeks (excluding transportation) and part of the costs is included in this project and part will be paid by LNA and SOAR. Additional details on this subject can be found in the document named STELES Design, that can be downloaded from the site: http://www.lna.br/~steles/Documents/steles-design.pdf

3.2 Instrument operation STELES will be operated in the same way as the other instruments on SOAR: by the

resident astronomers, in case of service observing or by the researcher itself, in the case of classical or remote operation. The SOAR support people will be trained by the STELES team during the commissioning. Presently, SOAR has 4 operators and 4 resident astronomers (3 Brazilians). The operation of the spectrograph is integrated with that of the telescope in the same virtual ambient (developed in LabView) to the point that anybody from anywhere in the world can use it through the Internet (under proper permission). The spectrograph was planned to have the smallest number of moving pieces as possible and will work in a fixed spectral configuration, in order that its operation will be the very easy, as compared with other instruments of the same class.

3.3 Maintenance plan As long as the operation, maintenance to prevent and correct failures will be performed by

SOAR support personnel, at SOAR expenses, with resources already allocated in the yearly budget, following plans prepared by the STELES team. The spectrograph is being developed in a way to minimize the impact on the work load and on the learning curve of the support personnel. It follows the standards defined by SOAR in terms of motors, connectors, electronics and cryostat. Regarding parts not compliant with SOAR standards, STELES team is preparing a list of replacement parts, that will be sent with the instrument. In the case of severe failures or miss-alignment (caused by strong earthquakes, for example) the STELES team will send a person to Pachon. Since it was

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designed to have high stability and few moving parts, little maintenance is expected along its life time.

In a few years in the future, it is possible that a upgrade of the instrument can be made, as long as there will be relevant technical advances (detectors, electronics, diffraction gratings) or new modules are required for specific purposes. The image acquisition software is the one already in use at SOAR. The data reduction package is being developed based on free platforms (Linux, Phyton, IRAF) and can be installed and receive support from SOAR support personnel.

4 – Management Approach

4.1-Construction Electronic and optical parts will be purchased from qualified companies, following criteria

of lowest price and best performance. Mechanical parts will be fabricated by LNA, when possible, or otherwise purchased from private companies. The team members will be in charge of the specification of the components, supervision of the fabrication/purchase, assemblage and tests, following the role of specific staff duties in the group. The coordinator is the final responsible for the project regarding FAPESP. A detailed description of the execution and management plan can be seen in the document: Steles Design (chapter 13) at: http://www.lna.br/~steles/Documents/steles-design.pdf. A few details in that document have been changed since the publication of the first version, but it remains essentially valid for the purpose of the present project submitted to FAPESP.

4.2- Technical management The management plan is based on the products of the project, the estimate of the costs and

time to be accomplished, including the actions for control of quality. The software Microsoft Project is used to develop and monitor the project calendar. The cost sheets generated in Microsoft Excel will be used to manage the costs. A risk analysis is in preparation, to optimize priorities, to predict weak points and to design a program of actions to minimize the impact of risks. In this document we present a preliminary and short version of the risk analysis pointing to most important points.

We maintain periodic meetings to evaluate the project development and to report solutions. E-mails, teleconferences and videoconferences are used to connect members of the team from different host institutions or when the physical presence of the members is not necessary.

4.3- Follow up and documentation The project follow up is made through a series of reviews organized by the instrument team

and coordinated by the SOAR Director, where independent specialists are put together to evaluate the project development. Two phases were already passed: a) the presentation of the proposal of the instrument to the SOAR Board of Directors (2002), when it was approved for studies and b) the Conceptual Design Review, when a detailed study of the instrument was presented to a committee composed by external reviewers from ESO (European Southern Observatory), CalTech (California Institute of Technology) and by representatives from the SOAR consortium. The project was approved with minor suggestions. There are 3 additional phases to occur: c) the Project Design Review, d) the Final Design Review and e) the Acceptance Test.

Every phase is documented by the instrument team and by the evaluators, the progress is reported in scientific meetings and published in papers. All the technical documents, including proposed maintenance, manual of operation, manual of software, and data reduction software will be delivered to SOAR. Copies and references to existing documents can be seen at: http://www.lna.br/~steles/resources.html

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4.4 – Financial Management The project expenditures will follow the project management plan and the funding schedule

presented in this project, and will be oriented in the best effort to guarantee the efficient use of the money and maintain the product quality. The project necessities will be responsibility of the Project Scientist/Manager Dr. Bruno Castilho (LNA) under agreement with the FAPESP project Principal investigator Dr. Augusto Damineli (IAG/USP).

FAPESP funds will be managed by FUSP (Fundação de Apoio a Universidade de São Paulo) foundation, following FAPESP procedures and supervised by the IAG/USP department of Astronomy contracts and agreements. All the financial reports and documentation will follow FAPESP procedures and will be provided to FAPESP by FUSP foundation under supervision of the project manager.

4.5 – Risk Analysis Risk factors can have detrimental implications in budget, schedule, and/or performance. As

said above, a risk analysis is in preparation following the detailing of the design to predict weak points and to develop mitigation strategies for areas of significant risk in the further design, manufacture, assembly, and commissioning phases of STELES. Here we present a summarized version of the analysis.

The risk factors in the project could be categorized as scientific, design, manufacture, assembly, and management risks. Scientific risks are risks that compromise the scientific performance or timeliness of the instrument. Design risks are areas of the instrument design that are yet to be clearly defined and which may prove not to be feasible. Manufacture risks are risks associated with the manufacture of the instrument. Assembly risks are the risks associated with, for example, achieving satisfactory alignment of the optics and reaching the required operating temperature. Management risks are risks associated with staff turnover, sickness, and availability, and project logistics.

Below we state the risks pointed by the STELES review panel and the approach for mitigating the risk taken by STELES team.

- Use of holographic gratings as crossdispersers – Design risk. Action – prototype gratings and test. Status – done, passed.

- Small separation of bluest orders can affect sky subtraction. Design risk. Action – improve design, test for reduction process. Status – done, passed with limitations

- Provide adequate guiding since STELES can not use SOAR guide facility without modifications. Design risk. Action – change mechanical design. Status – to be done in the detailing design (this proposal).

- Obtaining adequate coating for lenses and mirrors due STELES broad band coverage. Manufacture risk. Action – Order coating samples and test them. Status – ongoing.

- Provide adequate alignment approach and tools. Assembly risk. Action – Optical designer B. Delabre performed an alignment study for STELES. Status – passed.

- Provide adequate technical personal for STELES design/production. Design/Manufacture risk. Action – As a federal institution LNA does not has autonomy for hiring personal and since FAPESP and other funding institutions do not allow hiring people using their funds we included in this proposal funding previsions for 3rd part contracts to supply technical functions on the project. This is not the best approach but is what can be done in the present funding status.

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- Provide adequate funding for STELES production – Manufacture risk. Action – Submit project funding proposals to funding agencies. Status – ongoing (this proposal).

4.6 LNA infrastructure for production and assembling STELES In the last years LNA have directed a large fraction of its resources in creating conditions to

the development of astronomical instrumentation, trying to increase the number of staff in this areas and creating the material infrastructure of laboratories.

We can point as major investment the construction of a new laboratory building intended for technological development. This includes an optical laboratory specialized in optical fibers for astronomy applications, an optical characterization laboratory including interferometric facility, filter & grating measurement experiment and a clean cabin; an adaptive optics laboratory, electronic and mechanical workshops and an integration room. The present infrastructure if not enough to produce all STELES parts is well equipped produce several mechanical parts and to measure and test all subcontracted and shelf acquired parts, and to successfully assembly the instrument. More about LNA laboratories and infrastructure can be found at http://www.lna.br/tecno/index.html

LNA is aware that the number of staff dedicated to instrument development is far from being adequate, and that this is a limiting factor to explore adequately the technological opportunities. In this sense LNA is working on partnerships with other institutions with complimentary resources to join efforts in common interests.

5 – Personnel

5.1 The instrument team and participants in the project Name Role in the Project Qualification Institution Augusto Damineli Principal investigator-

Coordinator Astronomer IAG/USP

Bruno V. Castilho Instrument Scientist Astronomer LNA/MCT Clemens D. Geneiding Optical subsystems coordinator Astronomer LNA/MCT Francisco Rodrigues Instrument Control System Electronic engineer LNA/MCT Vanessa B. Macanhan Mechanical Design Mechanical engineer LNA/MCT Paulo F. Silva Mechanical Fabrication Mechanical engineer LNA/MCT Beatriz Barbuy Participant astronomer IAG/USP João E. Steiner Participant astronomer IAG/USP Walter J. Maciel Participant astronomer IAG/USP Marcos Diaz Perez Participant astronomer IAG/USP Gustavo Porto Mello Participant astronomer OV/UFRJ Silvia C. Rossi Participant astronomer IAG/USP Nelson Vani Leister Participant astronomer IAG/USP Cássio Barbosa Participant astronomer UNIVAP Alexandre S. de Oliveira Participant astronomer UNIVAP José H. Groh Participant Posdoc IAG/USP Mairan Teodoro Participant PhD student IAG/USP * some temporary participants with grants and subcontracts, and former team members are not listed.

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5.2- Potential users STELES will be available to all Brazilians and to members of the SOAR consortium: NOAO

(EUA), Michigan University (EUA), University of North Carolina (EUA), Comunidade Astronomica de Chile (Chile). In order to have a sense of how many Brazilians would benefit from STELES, we listed all astronomers and graduate students that have applied in recent years for telescope time through LNA (OPD, Gemini South – GS, Gemini North – GN, and SOAR), demanding high or medium resolution spectroscopy. We present the list of 132 researchers in the table below, indicating the telescope and instrument they requested and project ID they submitted.

Name Family name Telesc. Instrument ID Institution Abilio Mateus GS GMOS 1984 IAG/USP Adriana Valio Roque da Silva OPD Coudé 2063 MACKENZIE Adriano Hoth Cerqueira GN GMOS 1654 UESC Alan Alves Brito GS GMOS 1980 IAG/USP Alberto Rodriguez-Ardila GN GMOS 1692 LNA/MCT Alex Carciofi OPD Coudé 2068 IAG/USP Alexandre Bortoletto SOAR GOODMAN 1828 UFSC Alexandre Zabot SOAR GOODMAN 2014 IAG/USP Alexandre S. de Oliveira OPD Coudé 1525 LNA/MCT Alvaro Alvarez Candal GS GMOS 1976 ON/MCT Ana Beatriz de Mello OPD Coudé 2067 ON/MCT André V. Escudero OPD Coudé 1811 IAG/USP Angela Cristina Krabbe SOAR GOODMAN 2015 UFSM Anselmo Augusto GS GMOS 1749 IAG/USP Antônio Kanaan GS GMOS 1983 UFSC Antonio A. Pereyra Quiros OPD Coudé 2072 IAG/USP Antônio M. Magalhães OPD Coudé 2072 IAG/USP Armando Domiciano de Souza Jr OPD Coudé 1805 IAG/USP Augusto Damineli Neto SOAR GOODMAN 2022 IAG/USP Aurea Garcia-Rissmann GS GMOS 1666 LNA/MCT Barbara Garcia Castanheira SOAR GOODMAN 2024 UFRGS Barbara Heliodora Gonçalvez OPD Coudé 2048 UFSaoCarlos Basílio X. Santiago GS GMOS 1646 UFRGS Beatriz Barbuy GS GMOS 1980 IAG/USP Bernardo Borges SOAR GOODMAN 1828 UFSC Bruno V. Castilho GN GMOS 1619 LNA/MCT Carlos Alberto O. Torres OPD Coudé 2093 LNA/MCT Carlos M. Dutra GS GMOS 1643 UECS Charles H. Bonatto GN GMOS 1586 UFRGS Claudia Winge GN GMOS 1614 Gemini Claudia Mendes de Oliveira GN GMOS 1992 IAG/USP Cláudia Vilega Rodrigues SOAR GOODMAN 2011 INPE/MCT Claudio B. Pereira SOAR GOODMAN 2002 ON/MCT Claudio H.F. Melo OPD Coudé 2093 ESO Cristiano da Rocha GN GMOS 1632 INPE/MCT Daniel Epitacio Pereira OPD Coudé 2067 ON/MCT Daniel Iunes Raimann GN GMOS 1577 ON/MCT Daniela Lazzaro GS GMOS 1976 ON/MCT Deidimar Alves Brissi OPD Coudé 1960 UNIVAP Denise R. Gonçalves GN GMOS 1877 INPE/MCT Deonisio Cieslinski SOAR GOODMAN 2011 INPE/MCT Dimitri A. Gadotti SOAR GOODMAN 2001 IAG/USP

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Dinah Moreira Allen OPD Coudé 2049 UFRJ/OV Domingos C. Rodrigues GN GMOS 1620 UFMG Eduardo Bica GN GMOS 1623 UFRGS Eduardo Janot-Pacheco OPD Coudé 2063 IAG/USP Eduardo Charles Vasconcelos GN GMOS 1654 ON/MCT Eduardo S. Cypriano GN GMOS 1992 LNA/MCT Fabio Besolin GN GMOS 1671 Hawai Fabricio Ferrari GN GMOS 1586 UFRGS Fausto K.B. Barbosa GS GMOS 1758 UFRGS Felipe de Oliveira Alves OPD Coudé 1499 UFMG Fernando Roig GS GMOS 1976 ON/MCT Francisco F.S. Maia SOAR GOODMAN 2009 UFMG Francisco Xavier de Araujo OPD Coudé 2068 ON/MCT François Cuisinier GS GMOS 1873 UFRJ/OV Gabriel A.P. Franco OPD Coudé 1499 UFMG Gabriel Rodrigues Hickel OPD Coudé 1960 UNIVAP Gastão C.B. Lima Neto GN GMOS 1988 IAG/USP Gerardo Juan Manuel Luna SOAR GOODMAN 2025 ON/MCT German A. Racca GS GMOS 1667 ON/MCT Germano R. Quast OPD Coudé 2093 LNA/MCT Gustavo de Araujo Rojas GS GMOS 1875 IAG/USP Henri Plana GN GMOS 1972 UESC Henrique Fraquelli GN GMOS 1577 UFRGS Henrique R. Schmitt GN GMOS 1614 UFSM Horácio A. Dottori GN GMOS 1742 UFGRS Iranderly Fernandes de Fernandes SOAR GOODMAN 1940 LNA/MCT Isaura Fuentes-Carrera GN GMOS 1632 IAG/USP Jane C. Gregório-Hetem GS GMOS 1754 IAG/USP Jaques R.D. Lepine SOAR GOODMAN 1849 IAG/USP João E. Steiner SOAR GOODMAN 2017 IAG/USP João Francisco C. Santos Jr SOAR GOODMAN 2009 UFMG João Rodrigo Souza Leão GN GMOS 1671 UFRGS Jorge Ramiro de La Reza GS GMOS 1667 ON/MCT Jose Dias do Nascimento Jr. OPD Coudé 1947 UFRN José Eduardo Telles GS GMOS 1679 ON/MCT José Henrique Groh OPD Coudé 1968 IAG/USP Jose Renan de Medeiros OPD Coudé 1709 UFRN Katia Cunha OPD Coudé 1915 ON/MCT Kepler de Souza Oliveira SOAR GOODMAN 2024 UFRGS Laerte Sodré Jr. GS GMOS 1980 IAG/USP Lício da Silva OPD Coudé 1947 ON/MCT Luciano Fraga GS GMOS 1983 UFSC Mairan Teodoro GS GMOS 1884 IAG/USP Marcelo Borges Fernandes OPD Coudé 2068 UFRJ/OV Marcio A.G. Maia SOAR GOODMAN 2035 ON/MCT Marcos Perez Diaz SOAR GOODMAN 2011 IAG/USP Marcus Vinicius Massa Fernandes OPD Coudé 1898 IAG/USP Marcus Vinicius F. Copetti SOAR GOODMAN 2015 UFRGS Maria Auxiliadora Machado OPD Coudé 1511 ON/MCT Maria Jaqueline Vasconcelos GN GMOS 1871 UESC Mariangela de Oliveira-Abans SOAR GOODMAN 1835 LNA/MCT Maximiliano Faundez-Abans SOAR GOODMAN 1835 LNA/MCT

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Miriani Griselda Pastoriza GN GMOS 1586 UFRGS Monica M.M. Uchida GN GMOS 1636 IAG/USP Natalia Boris GN GMOS 1631 ON/MCT Natalia Vale Asari GN GMOS 1692 UFSC Nelson V. Leister OPD Coudé 1916 IAG/USP Odilon Giovannini GS GMOS 1983 UFCS Pamela de Paula Piovezan GN GMOS 1992 IAG/USP Patricia Cardoso Cruz OPD Coudé 2063 MACKENZIE Patricia Eiko de Campos GN GMOS 1677 IAG/USP Patricio Lagos GS GMOS 1873 ON/MCT Paula R.T. Coelho GS GMOS 1980 IAG/USP Paulo S. Pellegrini SOAR GOODMAN 2035 ON/MCT Raymundo Baptista SOAR GOODMAN 2014 UFSC/SOAR Ricardo L.C. Ogando SOAR GOODMAN 2035 UFRJ Roberto Cid Fernandes GN GMOS 1614 UFSC Roberto D.Dias da Costa SOAR GOODMAN 2025 IAG/USP Rocío M. Melgarejo Yrupailla OPD Coudé 1918 IAG/USP Rodolfo Henrique S. Smiljanic GS GMOS 1980 INPE/MCT Rogerio Riffel GS GMOS 1755 UFRGS Ronaldo Eustaquio de Souza SOAR GOODMAN 2001 IAG/USP Ronaldo S. Levenhagen OPD Coudé 1916 IAG/USP Sandra dos Anjos SOAR GOODMAN 2001 IAG/USP Sandro Javiel GS GMOS 1646 UFRGS Sandro Barboza Rembold GN GMOS 1586 UFRGS Sarita Pereira Carvalho OPD Coudé 1960 UNIVAP Sergio Scarano Jr. OPD Coudé 2055 IAG/USP Silvia Lorenz Martins OPD Coudé 2067 UFRJ/OV Simone Daflon OPD Coudé 1915 ON/MCT Slobodan Jankov OPD Coudé 1805 IAG/USP Thais E.P. Idiart SOAR GOODMAN 2010 IAG/USP Thaisa Storchi-Bergmann GN GMOS 1614 UFRGS Tiago Ricci GN GMOS 1990 IAG/USP Vera Jatenco-Pereira GN GMOS 1563 IAG/USP Vinicius de Abreu Oliveira SOAR GOODMAN 2015 UFSM Vinicius Schmidt M. Bordalo GS GMOS 1881 ON/MCT Wagner Jose Corradi Barbosa SOAR GOODMAN 2009 UFMG Walter J. Maciel SOAR GOODMAN 1827 IAG/USP Wilton S. Dias OPD Coudé 2048 UNIVAP

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6 –Budget We present an estimate to the cost of the instrument, based on the existing optical and

mechanical design. We quoted the parts based on the approximate characteristics that may change slightly as the detailed final design is done. Other sources of uncertainties can change the costs, but we believe that not to a large amount.

Project Components as considered by FAPESP forms Details in

Value

Permanent equipment acquired in Brasil Form 01 R$ 8370,00Permanent equipment acquired in other countries Form 02 US 5100,00Non permanent material to be acquired in Brasil Form 03 R$ 339.250,00Non permanent material to be acquired in other countries Form 04 US 227.350,003rd part services to be performed in Brasil Form 05 R$ 150.000,003rd part services to be performed in other countries Form 06 US 79.200,00Transportation costs – tickets Form 07 R$ 20.220,00Transportation costs – diaries Form 08 R$ 53.825,00 Total in US$ US 311.650,00Total in R$ R$ 571.665,00Grand total converting US$ (x2.1) in R$ R$ 1.226.130,00

The amount requested above to FAPESP corresponds to ~60% of the total cost of the instrument and is sufficient for its completion. A fraction of the STELES cost was already paid by the Instituto do Milênio (MEGALIT), by the FAPEMIG foundation, CNPq foundation and by the LNA, as show below.

Other funding for STELES - Milênio, 2 CCD Detectors, 2 Cryostats US$ 308.848,00 - Milênio, 1 electronic controller US$ 18.525,87 - Milênio, Mechanical Project by LEG Engenharia R$ 59.720,00 - Milênio, consultants, travel and others R$ 40.000,00 - Milênio, prototype holographic gratings US$ 8.500,00 - LNA, 2 R4 echelle gratings US$ 89.000,00 - LNA, 1 electronic controller US$ 23.000,00 - LNA, travel and other expenses R$ 15.000,00 - CNPq, Coatings and dicrhoic tests R$ 34.500,00 - FAPEMIG, software, laboratory instruments R$ 105.000,00

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7- Simplified Schedule – indicating principal stages and estimate time. Simplified STELES Project Schedule

Time - expressed in 3months bin (year1 / 3months bin 1) 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4

Mechanical Project Detailing Control system and electronics detailing Optical procurement Project Design Review PDR Report answering and fixing Error budget and Risk analysis Mechanical Drawings for production Critical Design review Optical components acquisition Mechanical parts production On shelf mechanical parts acquisition In house (LNA) mechanical production Acceptance and tests Integration, Alignment Bench tests Acceptance tests Transport Commissioning

8- Outreach We plan to built a homepage dedicated to Spectral Analysis for students and interested

public. The idea is to present the basic concepts, the historical developments and the use of spectroscopy in Astronomy. The homepage intend to be interactive, showing examples of radial velocity measurements, used for binary stars, planetary motions, redshifts etc. In particular, we will offer self-testing on stellar and nebular spectral classification. The necessary funds will come from the grant associated with the project and therefore, it was not included in the budget.

9- Bibliography

9.1- Technical Publications

• A new concept for echelle spectrographs: the SOAR Telescope Echelle Spectrograph, 2004, Castilho, Bruno V.; Delabre, Bernard; Gneiding, Clemens D. Ground-based Instrumentation for Astronomy. Edited by Alan F. M. Moorwood and Iye Masanori. Proceedings of the SPIE, Volume 5492, pp. 433-444 (2004). (SPIE Homepage)

• New solution in echelle crossdispersing - the soar telescope echelle spectrograph, 2004, Castilho, B. V.; Delabre, B.; Gneiding, C. D.; Tull, R. G., Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p.195-195

• The Soar Telescope Echelle Spectrograph - STELES, 2003, B. V. Castilho, C. D. Gneiding, B. Delabre, Optical and Infrared Astronomical Instrumentation for Modern Telescopes - Brazilian Workshop Editors - Bruno V. Castilho & Clemens D. Gneiding Location - Angra dos Reis, Rio de Janeiro, Brazil Date - November 16-20, 2003 Publisher - Laboratorio Nacional de Astrofisica Proceedings - published on CD-ROM ISBN - 85-98138-01-0

• STELES Management Plan, 2003, C.R.G. Andrade, Optical and Infrared Astronomical Instrumentation for Modern Telescopes - Laboratorio Nacional de Astrofisica Proceedings - published on CD-ROM ISBN - 85-98138-01-0

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• SOAR Telescope Echelle Spectrograph control system: the user interface, 2003, L.B. Delefrate, B.V. Castilho, Optical and Infrared Astronomical Instrumentation for Modern Telescopes - Laboratorio Nacional de Astrofisica Proceedings - published on CD-ROM ISBN - 85-98138-01-0

• The temperature control system for STELES spectrograph, 2003, O. Giovannini, B.V. Castilho, Optical and Infrared Astronomical Instrumentation for Modern Telescopes - Laboratorio Nacional de Astrofisica Proceedings - published on CD-ROM ISBN - 85-98138-01-0

• An Exposure Time Calculator for the SOAR Telescope Echelle Spectrograph, 2003, R.Y.Z. Sediyama, B.V. Castilho, Optical and Infrared Astronomical Instrumentation for Modern Telescopes - Laboratorio Nacional de Astrofisica Proceedings - published on CD-ROM ISBN - 85-98138-01-0

• Online data reduction software for the STELES Spectrograph, 2003, M. J. Vasconcelos, Bruno V. Castilho, A.H. Cerqueira, Optical and Infrared Astronomical Instrumentation for Modern Telescopes - Laboratorio Nacional de Astrofisica Proceedings - published on CD-ROM ISBN - 85-98138-01-0

• STELES Contribution for heavy elements abundances determination, 2003, D. Moreira-Allen, B. Barbuy, Optical and Infrared Astronomical Instrumentation for Modern Telescopes - Laboratorio Nacional de Astrofisica Proceedings - published on CD-ROM ISBN - 85-98138-01-0

9.2- Sample of science papers

• Alves-Brito, A., Barbuy, B., Ortolani, S., Momany, Y., Hill, V., Zoccali, M., Renzini, A., Pasquini, L., Minniti, D., Bica, E., Rich, R.M., A&A, 435, 657, 2005

• Barbuy, B, Zoccali, M, Ortolani, S., Momany, Y., Minniti, D., Hill, V, Renzini, A., Rich, R.M., Bica, E., Pasquini, L., Yadav:, R.K.S., A&A, 449, 349, 2006

• Barbuy, B., Spite, M., Spite, F., Hill, V., Cayrel, R., Plez, B., Petitjean, P,: 2005, A&A, 429, 1031, 2005

• Barklem, P. S., Christlieb, N., Beers, T. C.; Hill, V., Bessell, M. S., Holmberg, J., Marsteller, B., Rossi, S., Zickgraf, F.-J., and Reimers, D. 2005, A&A 439, 129, 2005

• Casey, B.W., Mathieu, R.D., Vaz, L.P.R., Andersen, J., Suntzeff, N.B., AJ, 115, 1617, 1998

• Castilho, B.V., Spite, F., Barbuy, B., Spite, M., De Medeiros, J.R., Gregorio-Hetem, J., A&A, 345, 249, 1999

• Castro, S., Porto de Mello, G. F., da Silva, L., MNRAS, 305, 693, 1999

• Cayrel, R., Depagne, E., Spite, M., Hill, V., Spite, F., Francois, P., Plez, B., Beers, T., Primas, F., Andersen, J., Barbuy, B., Bonifacio, P., Molaro, P., Nordstrom, B., A&A, 416, 1117, 2004

• Cayrel, R., Hill, V., Beers, T., Barbuy, B., Spite, M., Spite, F., Plez, P., Andersen, J., Bonifacio, P., Francois, P., Molaro, P., Nordstrom, B., Primas, F., Nature, 409, 691, 2001

• Daflon, S. & Cunha, K., ApJ 617, 1115, 2004

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• Daflon, S., Cunha, K., Butler, K., & Smith, V.V. , ApJ 563, 325, 2001

• Daflon, S., Cunha, K., & Butler, K., ApJ 604, 362, 2004

• Damineli, A., ApJ, 460, L49, 1996

• Diaz, M.P. and Ribeiro, F., AJ, 125, 3359, 2003

• Diaz, M. P., ApJ, 553, L177, 2001

• Floquet, M., Neiner, C., Janot-Pacheco, E., Hubert, A. M.; Jankov, S., Zorec, J., Briot, D., Chauville, J., Leister, N. V., Percy, J. R., A&A, 394,137, 2002

• Gregorio-Hetem, J. and Hetem, A., MNRAS 336, 197, 2002

• Groh, J.H., Hillier, D.J. and Damineli, A., ApJ, 538, L33, 2006

• Korn, A. J., Nieva, M. F., Daflon, S. & Cunha, K., ApJ 633, 899, 2005

• Levenhagen, R..S., Leister, N.V., Janot-Pacheco, E., Zorec, J., Hubert, A.M., and Floquet, M., A&A 400, 599, 2003

• Lucatello, S., Beers, T. C., Christlieb, N., Barklem, P. S., Rossi, S., Marsteller, B., Sivarani, T., and Lee, Y. S., ApJ 652, 37L, 2006

• Maciel, W.J., Lago, L.G., and Costa, R.D.D., A&A 453, 587, 2006

• Pereira, C. B. & Roig, F. ,A&A, 452, 571, 2006

• Pereira, C. B., Lorenz-Martins, S. and Machado, M., A&A. 422, 637, 2004.

• Rocha-Pinto, H.J, Scalo, J., Maciel, W.J. and Flynn, C., ApJ 531, L115, 2000

• Rojas, G., Gregorio-Hetem, J., in Cool Stars, Stellar Systems and the Sun 13 , 2005

• Rossi, S.; Beers, T. C.; Sneden, C.; Sevastyanenko, T.; Rhee, J.; and Marsteller, B., AJ 130. 2804, 2005

• Steiner, J.E., and Damineli, A., ApJ, 612, L133, 2004

• Torres, C.A., Quast, G.R., da Silva, L., de la Reza, R., Melo, C.H.F. and Sterzik - astro-ph/0609258

• Vinicius,M.M.F.;Zorec,J.;Leister, N. V., and Levenhagen, R.S., A&A, 446, 643, 2006

• Pogodin, M. A.; Franco, G. A. P.; and Lopes, D. F., A&A, 438, 239, 2005

• Pogodin, M. A.; Malanushenko, V. P.; Kozlova, O. V.; Tarasova, T. N.; and Franco, G. A. P., A&A, 452, 551, 2006

• Torres, K.B., and Vaz, L.P.R., IAU Symposium, 240, 2006

• Vieira, S. L. A.; Pogodin, M. A.; and Franco, G. A. P., A&A, 345, 559, 1999

• Zoccali, M., Lecureur, A., Barbuy, B., Hill, V., Renzini, A., Minniti, D., Gomez, A., Ortolani:, S., A&A Letters- accepted

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Appendix A

Justification of the budget following the items entered in the FAPESP spread sheets

FORM 1

EQUIPMENT TO BE PURCHASED IN BRAZIL

1- Electronic controller module for positioning the motors – from National Instruments. The motors specified for the STELES spectrograph are intelligent, with built-in controllers. The module defined in this item will integrate all motors controls.

2-Microcomputer to control the spectrograph. STELES design demands a PC computer to run the software and interfaces to control the spectrograph. 3- Expenses with handling & shipping. These equipment are made in USA but will be purchased through a Brazilian company.

FORM 2

EQUIPMENT TO BE IMPORTED 1 - Cooled CCD camera for guiding – made in USA. Among other control functions, the star must be kept inside the 2 slits of the spectrograph. To perform this task, we will use two thermoelectrically cooled cameras. Thermoelectrically cooled cameras (Peltier effect) is adequate for guiding on 17th magnitude stars. We chose the ST7 SBIG as the optimal cost/benefit for the project. 2- Expenses with handling & shipping The equipment will be imported from USA

FORM 3

ITEMS AND SUPPLIES TO BE PURCHASED IN BRAZIL 1- 450 mechanical parts of the spectrograph, to be produced under specifications of the project, contracted from Brazilian factories. Only a few items are available off the shelf. The major part of the mechanical components will be built following STELES design specifications and fabricates by companies with expertise in precision mechanics.

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2 – Materials for fabrication of mechanical components are available at LNA mechanical shop, at no additional cost for the project. A set of mechanical pieces, those of lower tolerances, can be built in this way. The others will be ordered from local companies. 3 –Tools for computer controlled milling machine. In order to build some pieces, we need to

upgrade the present capabilities of the LNA milling machine. Even computing the expenses of the

acquisition of the tools, the final cost of the pieces will be cheaper than ordering from industries.

4 - Electric and electronic cables, connectors and other components for the spectrograph integration. The cables will provide electric power and electronic signals among the subsystems of the spectrograph and the corresponding control module and computers. A subset of the cables will be installed inside the mechanical bench of the spectrograph and others will be located outside. The connectors will be selected in accordance with SOAR standards, in order to facilitate maintenance and replacement. In cases where a specific connector will not be compliant with SOAR requirements, we will provide spare parts. 5 - Temperature sensors with 0.1C accuracy. The spectrograph will be kept at constant temperature with a accuracy of 0.25 C, at least for a period of 4 hours. 6 - Expenses with handling, shipping and importation (items 1 and 2 have this cost included). The equipment will be imported from USA

FORM 4

ITEMS AND SUPPLIES TO BE IMPORTED 1 – Set of mirrors (flat and for the collimator) to be fabricated in USA under specification of the project. Set of collimating and flat mirrors to be ordered in USA. Those are 7 high precision mirrors, 2 spherical, 2 parabolic and 3 flat, to be fabricated under specification of the project. The mirror designs can be found in the STELES homepage in the Design Document. 2 - Set of lenses and prisms for the fore-optics, to be fabricated in USA under specification of the project Set of lens and prisms for the fore-optics to be fabricated under specifications of the project, in USA. Those correspond to 11 high precision lenses and 2 prisms. The design of lenses and prisms can be found in the STELES Design Document. 3 - Optics for the blue and red cameras, including the assembling cells, to be fabricated in USA under specification of the project Optics for the red and blue cameras of the spectrograph, including the lens mounts. To be purchased in USA. Those correspond to 8 high precision lenses in the red camera and 7 in the blue camera. Fabricated under project specification using high quality glasses. Due to the very high precision optics, the international review panel suggested that the mounts for the lenses should be made in the factory that will produce the lenses. In this way, the cost of mounts and alignment are included. The design of lenses and their respective specifications can be found in the STELES homepage and Design Document.

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4 – 2 cross-dispersers diffraction gratings, to be fabricated in USA, under specification of the project 2 holographic gratings, with 600 l/mm and 1500 l/mm, operating in the wavelength range 530-900nm and 300-530nm respectively. Two of those gratings were already prototyped by Wasatch Photonics (USA), in order to test the fabrication technology in the UV spectral range – never done before this project. The prototypes passed the tests made at ESO. In this item, we specify the 2 final gratings for STELES, under the specifications of the optical design. 5 - Dichroic filter with lambda/10 flatness, reflecting in the spectral range 300-530nm and transmitting in the range 530-900nm (USA) It will be used to split the light beam. Detailed specification projected by BARR Associates (USA) can de found in the STELES homepage. 6 - Honeycomb and materials for the fabrication the spectrograph optical bench (made in USA). The bench material is composed of carbon fiber skin, mounted in a metal honeycomb and capable of delivering high stiffness and low weight. A company of high precision standards will build the optical bench in Brazil, but the carbon fiber material must be imported. 7 - Linear guides and actuators for high precision mechanical positioning (USA) Such high precision mechanical guiding are not fabricated in Brazil and must be imported. 8 – Circular stage for high precision mechanical positioning (USA) Such high precision mechanical components are not fabricated in Brazil and must be imported. 9 – 2-axix linear stages (USA) High precision mechanical systems for the positioning of optical components are not fabricated in Brazil and must be imported 10 – 10 step motors for positioning, to be ordered in USA, under the standards defined by the SOAR project SmartMotors are fabricated by Qcontrol company (USA) and follow the specifications made by SOAR for better operationally and maintenance. 11 – 10 motor controllers (plus the corresponding interfaces), to be ordered in USA, under the standards defined by SOAR Those are electronic controllers for the above mentioned motors. 12 – 10 Breakout modules for 10 motors (USA) Breakout electronic modules for the motors mentioned above. 13 – Clamp Module National (USA) Electronic module to interconnect the controllers of all motors of the spectrograph. 14 – Power supplies for the motors of item 10 (USA) Electric energy sources for the above mentioned motors. 15- Expenses with handling & shipping for all items in this form The equipment will be imported from USA

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FORM 5

THIRD PART LABOR 1 – Labor hours for fabricating the mechanical parts of the spectrograph We ask funds for paying the fabrication of mechanical parts of the spectrograph. A fraction of the pieces will be fabricated at the LNA shops in order to speed up the completion of the project. 2 – Labor to [built] build the optical bench of the spectrograph The optical bench of STELES is built in aluminum, filled with carbon fiber parts. This demands specific technology available in a São Paulo state factory. 3 – Anodization of the mechanical parts of the spectrograph Black anodization of all the mechanical parts to minimize the internal light reflection. This requires a specialized company, available in Brazil. 4 – Consulting time for the mechanical project The main work for the mechanical project will be executed at LNA, but for critical parts we will need to contract an external mechanic engineer, expert in opto-mechanics to revise and design specific piece/assembly design. 5 – Fabrication of the special cases for transportation of the instrument to Pachon The instrument is fragile, is big (1,6 x 1,8 x 0.6 m) and weighs ~800Kg, in order that a special case must be built for transportation to Chile. 6 – Transportation cost of the spectrograph to Pachon (Chile). The instrument, after integrated and accommodate in the case, will be transported by land and air from the LNA laboratory (Minas Gerais) to Cerro Pachon (Chile).

FORM 6

THIRD PART LABOR to be contracted outside Brazil 1 – Anti-reflection coating for the lenses (USA) Multilayer coating to reduce light reflections on the lenses from 8% to <1%. There are no companies with such capability in Brazil. 2 –Reflection coating for the mirrors (USA) Coatings to enhance the reflectivity of the mirrors from 90% to 96%. There are no companies with such capability in Brazil. 3 – Specialized consultants for the optical design (hours). STELES optical design was made by Dr. Bernard Delabre from ESO, funded by Instituto do Milênio. The details of the opto-mechanical components must be designed by a specialized engineer. He will deliver the fabrication design, including fabrication tolerances, scattered light inside the instrument and final revision of the optical design. 4- Specialized consultants for the mechanical project (hours) The main parts of the mechanical design will be accomplished by a LNA mechanical engineer.

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However, some critical parts and the final revision of the mechanical design must be done by a person with skills in opto-mechanics for scientific instruments, not available in Brazil.

FORM 7

TRAVEL EXPENSES 1 - National flight tickets for meetings of the project team members The team members are from different Brazilian Institutions and need to meet from time to time to follow the development of the project. 2 – International flight tickets for meetings with specialists The complexity of the instrument demands meetings for technical discussion with foreign specialists and contracted companies that will built parts of the instrument. 3 – National flight tickets for meetings with specialists Since some parts of the instruments are built by Brazilian companies, some meetings for discussions with specialists and companies will be done.

FORM 8

DAILY EXPENSES 1 – Daily expenses in São Paulo and Rio de Janeiro for meetings of the project team. To pay the hotel & meals expenses of the team members when meetings are made in Rio de Janeiro or São Paulo. 2 – Daily expenses in Itajubá and other cities, for meetings of the project team To pay the hotel & meals expenses of the team members when meetings are made in Itajubá or other small Brazilian city. 3 – Daily expenses for technical meetings with factories in São Paulo To pay the hotel & meals expenses in the occasion of technical meetings in São Paulo factories. 4 – Daily expenses for technical meetings in other Brazilian cities To pay the hotel & meals expenses in the occasion of technical meetings in factories of small cities in Brazil. 5 – International daily expenses for technical meetings To pay the hotel & meals expenses in the occasion of technical meetings with specialists and companies outside Brazil.

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Appendix B

Letter from SOAR accepting the STELES project