A. Marín-Franch

Centro de Estudios de Física del Cosmos de Aragón, Terol, Aragon, Spain

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Publications (70)146.6 Total impact

  • S. Reichel, U. Brauneck, S. Bourquin, A. Marín-Franch
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    ABSTRACT: The Observatorio Astrofisico de Javalambre in Spain observes with its telescope galaxies in the Local Universe plans to perform a multi-band survey, where optical filters are needed. Different filters with a full width half maximum between 10-20 nm with central wavelengths at 395 nm, 410 nm, 430 nm, 515 nm, and an average transmission Tave larger than 85 % in the passband and blocking from 250 nm to 1050 nm of OD5 (T < 10-5) will be shown. The edges are steep for a narrow transition from 5 % to 80 % and the transmitted wavefront error of the optical filter are less than λ/2 over an aperture > 100 mm.
    SPIE Astronomical Telescopes + Instrumentation; 08/2014
  • SPIE Astronomical Telescopes + Instrumentation; 07/2014
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    ABSTRACT: The Observatorio Astrofísico de Javalambre in Spain is a new astronomical facility particularly conceived for carrying out large sky surveys with two unprecedented telescopes of unusually large fields of view: the JST/T250, a 2.55m telescope of 3deg field of view, and the JAST/T80, an 83cm telescope of 2deg field of view. The most immediate objective of the two telescopes for the next years is carrying out two unique photometric surveys of several thousands square degrees, J-PAS[9][14][16] and J-PLUS [14][16], each of them with a wide range of scientific applications, like e.g. large structure cosmology and Dark Energy, galaxy evolution, supernovae, Milky Way structure, exoplanets, among many others. To do that, JST and JAST will be equipped with panoramic cameras under development within the J-PAS collaboration, JPCam and T80Cam respectively, which make use of large format (~ 10k x 10k) CCDs covering the entire focal plane. This paper describes in detail the engineering development of the overall facilities and infrastructures for the robotic observatory and a global overview of current status and future actions to perform from engineering point of view.
    SPIE Astronomical Telescopes + Instrumentation; 07/2014
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    S. Ramírez Alegría, A. Marín-Franch, A. Herrero
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    ABSTRACT: The discovery of new, obscured massive star clusters has changed our understanding of the Milky Way star-forming activity from a passive to a very active star-forming machine. The search for these obscured clusters is strongly supported by the use of all-sky, near-IR surveys. The main goal of the MASGOMAS project is to search for and study unknown, young, and massive star clusters in the Milky Way, using near-IR data. Here we try to determine the main physical parameters (distance, size, total mass, and age) of Masgomas-4, a new double-core obscured cluster. Using near-IR photometry ($J$, $H$, and $K_S$) we selected a total of 21 stars as OB-type star candidates. Multi-object, near-IR follow-up spectroscopy allowed us to carry out the spectral classification of the OB-type candidates. Of the 21 spectroscopically observed stars, ten are classified as OB-type stars, eight as F- to early G-type dwarf stars, and three as late-type giant stars. Spectroscopically estimated distances indicate that the OB-type stars belong to the same cluster, located at a distance of $1.90^{+1.28}_{-0.90}$ kpc. Our spectrophotometric data confirm a very young and massive stellar population, with a clear concentration of pre-main-sequence massive candidates (Herbig Ae/Be) around one of the cluster cores. The presence of a surrounding HII cloud and the Herbig Ae/Be candidates indicate an upper age limit of 5 Myr.
    05/2014;
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    ABSTRACT: There are many ways to solve the challenging problem of making a high performance robotic observatory from scratch. The Observatorio Astrof\'isico de Javalambre (OAJ) is a new astronomical facility located at the Sierra de Javalambre (Teruel, Spain) whose primary role will be to conduct all-sky astronomical surveys. The OAJ control system has been designed under a global point of view including not only astronomical subsystems but also infrastructure and other facilities. Three main factors have been considered in the design of a global control system for the robotic OAJ: quality, reliability and efficiency. We propose CIA (Control Integrated Architecture) design and OEE (Overall Equipment Effectiveness) as a key performance indicator in order to improve operation processes, minimizing resources and obtain high cost reduction maintaining quality requirements. The OAJ subsystems considered for the control integrated architecture are the following: two wide-field telescopes and their instrumentation, active optics subsystems, facilities for sky quality monitoring (seeing, extinction, sky background, sky brightness, clouds distribution, meteorological station), domes and several infrastructure facilities such as water supply, glycol water, water treatment plant, air conditioning, compressed air, LN2 plant, illumination, surveillance, access control, fire suppression, electrical generators, electrical distribution, electrical consumption, communication network, Uninterruptible Power Supply and two main control rooms, one at the OAJ and other remotely located in Teruel at 40km from the observatory, connected through a microwave radio-link. Here we present the OAJ strategy in control design to achieve maximum quality efficiency for the observatory processes and operations, giving practical examples of our approach.
    Proc SPIE 04/2014;
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    ABSTRACT: The Javalambre-Physics of the Accelerated Universe Astrophysical Survey (J-PAS) is a narrow band, very wide field Cosmological Survey to be carried out from the Javalambre Observatory in Spain with a purpose-built, dedicated 2.5m telescope and a 4.7 sq.deg. camera with 1.2Gpix. Starting in late 2015, J-PAS will observe 8500sq.deg. of Northern Sky and measure $0.003(1+z)$ photo-z for $9\times10^7$ LRG and ELG galaxies plus several million QSOs, sampling an effective volume of $\sim 14$ Gpc$^3$ up to $z=1.3$ and becoming the first radial BAO experiment to reach Stage IV. J-PAS will detect $7\times 10^5$ galaxy clusters and groups, setting constrains on Dark Energy which rival those obtained from its BAO measurements. Thanks to the superb characteristics of the site (seeing ~0.7 arcsec), J-PAS is expected to obtain a deep, sub-arcsec image of the Northern sky, which combined with its unique photo-z precision will produce one of the most powerful cosmological lensing surveys before the arrival of Euclid. J-PAS unprecedented spectral time domain information will enable a self-contained SN survey that, without the need for external spectroscopic follow-up, will detect, classify and measure $\sigma_z\sim 0.5\%$ redshifts for $\sim 4000$ SNeIa and $\sim 900$ core-collapse SNe. The key to the J-PAS potential is its innovative approach: a contiguous system of 54 filters with $145\AA$ width, placed $100\AA$ apart over a multi-degree FoV is a powerful "redshift machine", with the survey speed of a 4000 multiplexing low resolution spectrograph, but many times cheaper and much faster to build. The J-PAS camera is equivalent to a 4.7 sq.deg. "IFU" and it will produce a time-resolved, 3D image of the Northern Sky with a very wide range of Astrophysical applications in Galaxy Evolution, the nearby Universe and the study of resolved stellar populations.
    03/2014;
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    arXiv:1403.5237. 03/2014;
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    ABSTRACT: We study the characteristics of a narrow band type Ia supernova survey through simulations based on the upcoming Javalambre Physics of the accelerating universe Astrophysical Survey (J-PAS). This unique survey has the capabilities of obtaining distances, redshifts, and the SN type from a single experiment thereby circumventing the challenges faced by the resource-intensive spectroscopic follow-up observations. We analyse the flux measurements signal-to-noise ratio and bias, the supernova typing performance, the ability to recover light curve parameters given by the SALT2 model, the photometric redshift precision from type Ia supernova light curves and the effects of systematic errors on the data. We show that such a survey is not only feasible but may yield large type Ia supernova samples (up to 300 supernovae at $z<0.5$ per month of search) with low core collapse contamination ($\sim 3$ per cent), good precision on the SALT2 parameters (average $\sigma_{m_B}=0.063$, $\sigma_{x_1}=0.47$ and $\sigma_c=0.040$) and on the distance modulus (average $\sigma_{\mu}=0.17$, assuming an intrinsic scatter $\sigma_{\mathrm{int}}=0.14$), with identified systematic uncertainties $\sigma_{\mathrm{sys}}\lesssim 0.10 \sigma_{\mathrm{stat}}$. Moreover, the filters are narrow enough to detect most spectral features and obtain excellent photometric redshift precision of $\sigma_z=0.005$, apart from $\sim$ 2 per cent of outliers. We also present a few strategies for optimising the survey's outcome. Together with the detailed host galaxy information, narrow band surveys can be very valuable for the study of supernova rates, spectral feature relations, intrinsic colour variations and correlations between supernova and host galaxy properties, all of which are important information for supernova cosmological applications.
    Monthly Notices of the Royal Astronomical Society 12/2013; 444(3). · 5.52 Impact Factor
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    ABSTRACT: In this study we compare the photometric data of 34 Milky Way globular clusters, observed within the ACS Treasury Program (PI: Ata Sarajedini) with the corresponding ground-based data, provided by the Photometric Standard Field Catalogs of Stetson (2000, 2005). We focus on the transformation between the HST/ACS F606W to V-band and F814W to I-band only. The goal is to assess the validity of the filter transformation equations by Sirianni et al.(2005) with respect to their dependence on metallicity, Horizontal Branch morphology, mass and integrated (V-I) colour of the various globular clusters. Such a dependence is expected due to the fact that the transformation equations are based on the observations of only one globular cluster, i.e., NGC 2419. Surprisingly, the correlation between offset and metallicity is found to be weak, with a low level significance. The correlation between offset and Horizontal Branch structure, as well as total cluster mass is still weaker. Based on the available data we do not find the photometric offset to be linked to multiple stellar populations, e.g., as found in NGC 0288, NGC 1851, and NGC 5139. The results of this study show that there are small systematic offsets between the transformed ACS- and observed ground based photometry, and that these are only weakly correlated, if at all, with various cluster parameters and their underlying stellar populations. As a result, investigators wishing to transform globular cluster photometry from the Sirianni et al.(2005) ground-based V, I system onto the Stetson (2000) system simply need to add 0.040 (+/-0.012) to the V-band magnitudes and 0.047 (+/-0.011) to the I-band magnitudes. This in turn means that the transformed ACS (V-I) colours match the ground-based values from Stetson (2000) to within ~0.01 mag.
    The Astrophysical Journal Supplement Series 12/2013; 211(1). · 16.24 Impact Factor
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    ABSTRACT: We are carrying out a systematic search for Lyman Break Galaxies (LBGs) in the ALHAMBRA Survey data. With the ALHAMBRA filter set, we can detect the Lyman forest, permitting a LBG identification, for galaxies at redshifts z > 2 and up to z˜5 for the brightest objects. Our LBG candidate selection bases on spectral fitting of template spectra on the very low resolution spectra derived from the 20 intermediate optical band and three infrared broad band ALHAMBRA filters. The spatial coverage of ALHAMBRA survey (4 deg^2) is bigger than in any of the previous LBG surveys. The surface density of LBGs decreases with brightness so that we especially expect to contribute on better sampling of the bright end of the LBG luminosity function. Once the shallower, but much more extended (8000 deg^2) JPLUS and JPAS survey data are available, we will adopt our LBG search method to these surveys. Thanks to the huge area covered by these new surveys, we expect to achieve significant information on the bright LBGs at z˜2-3 (JPLUS) and z˜2-4 (JPAS).
    05/2013;
  • S. A. Ramírez Alegría, A. Herrero, A. Marín-Franch
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    ABSTRACT: We present two new massive clusters, discovered during the second phase of our MASGOMAS project (MAssive Stars in Galactic Obscured MAssive clusterS). The second phase of the project focuses on a systematic search of OB-type star candidates over-densities. We also present new near-infrared photometry (J, H, and K_S) and mid-resolution follow-up spectroscopy (H and K), obtained with LIRIS at ORM (La Palma), for the stellar content of the new massive clusters. With these data we have confirmed that Masgomas-1, the first candidate discovered by us, is a young and massive cluster, probably exceeding 10^4 {M}_{⊙}, which hosts both an OB-type and an RSG populations. We have also determined the cluster distance and extinction, placing it in the Scutum-Centaurus arm, but far from the arm base (where RSGC1, RSGC2, RSGC3, Alicante 8 and Alicante 10 clusters are located), and closer to the Sun. For our second new massive cluster candidate (Masgomas-4), we have spectroscopically confirmed the presence of a massive stellar population, and photometrically detected a group of massive pre-stellar objects (Herbig Ae/Be candidates). With the estimated individual distances for the cluster massive stars, we have derived a single distance for both cores, confirming that Masgomas-4 is a single young cluster.
    05/2013;
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    ABSTRACT: CIRCE is a near-infrared (1-2.5 μm) imager, polarimeter and low-resolution spectrograph intended as a visitor instrument for the Gran Telescopio Canarias.
    05/2013;
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    ABSTRACT: The Observatorio Astrofísico de Javalambre (OAJ) is a new Spanish astronomical facility particularly conceived for carrying out large sky surveys, making use of two unprecedented telescopes of unusually large fields of view (FoV): the JST/T250, a 2.55 m telescope of 3 deg FoV, and the JAST/T80, an 83 cm telescope of 2 deg FoV. After two years of project development, JAST/T80 is already installed at the OAJ undergoing the first performance tests, and JST/T250 is fully assembled in the factory awaiting for the completion of the optics. We here provide an overall description of the project, indicating the current status of the main work packages and the next future developments.
    Highlights of Spanish Astrophysics VII; 05/2013
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    ABSTRACT: The Observatorio Astrofísico de Javalambre (OAJ) is a new astronomical facility located at the Sierra de Javalambre (Teruel, Spain) whose primary role will be to conduct all-sky astronomical surveys. The OAJ facility will have two wide-field telescopes: the T250/JST; a 2.55-m telescope with a 3° diameter FoV, and the T80/JAST; a 0.83 m telescope with a 2° diameter FoV. In this poster the JAST/T80 and JST/T250 first light panoramic instruments are presented. T80Cam is a wide-field camera that will be mounted at the Cassegrain focus of the T80/JAST. It is intended for surveys, starting with the planned J-PLUS (Javalambre Photometric Local Universe Survey) survey, a twelve-band photometric all-sky survey. JPCam is a 14-CCD mosaic camera using the new e2v 9k-by-9k 10 μm pixel detectors, providing a pixel scale of 0.2"/pixel when mounted on the T250/JST. It is designed to perform the Javalambre-PAU Astrophysical Survey (J-PAS), a BAO survey of the northern sky. The J-PAS survey will use 57 filters, 54 narrow-band filters (˜13.8 nm) equi-spaced between 350 and 1000nm plus 3 broad-band filters to achieve unprecedented photometric red-shift accuracies for faint galaxies over ˜8000 square degrees of sky.
    Highlights of Spanish Astrophysics VII; 05/2013
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    ABSTRACT: JPCam is a 14-CCD mosaic camera, using the new e2v 9k-by-9k 10microm-pixel 16-channel detectors, to be deployed on a dedicated 2.55m wide-field telescope at the OAJ (Observatorio Astrofisico de Javalambre) in Aragon, Spain. The camera is designed to perform a Baryon Acoustic Oscillations (BAO) survey of the northern sky. The J-PAS survey strategy will use 54 relatively narrow-band (~13.8nm) filters equi-spaced between 370 and 920nm plus 3 broad-band filters to achieve unprecedented photometric red-shift accuracies for faint galaxies over ~8000 square degrees of sky. The cryostat, detector mosaic and read electronics is being supplied by e2v under contract to J-PAS while the mechanical structure, housing the shutter and filter assembly, is being designed and constructed by a Brazilian consortium led by INPE (Instituto Nacional de Pesquisas Espaciais). Four sets of 14 filters are placed in the ambient environment, just above the dewar window but directly in line with the detectors, leading to a mosaic having ~10mm gaps between each CCD. The massive 500mm aperture shutter is expected to be supplied by the Argelander-Institut fur Astronomie, Bonn. We will present an overview of JPCam, from the filter configuration through to the CCD mosaic camera. A brief outline of the main J-PAS science projects will be included.
    01/2013;
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    ABSTRACT: In this paper we present the results of image quality tests performed on the optical system of the Canarias InfraRed Camera Experiment (CIRCE), a visitor-class near-IR imager, spectrograph, and polarimeter for the 10.4 meter Gran Telescopio Canarias (GTC). The CIRCE optical system is comprised of eight gold-coated aluminum alloy 6061 mirrors. We present surface roughness analysis of each individual component as well as optical quality of the whole system. We found all individual mirror surface roughness are within specifications except Fold mirrors 1 and 2. We plan to have these components re-cut and re-coated. We used a flat 0.2-arcseconds pinhole mask placed in the focal plane of the telescope to perform the optical quality tests of the system. The pinhole mask covers the entire field of view of the instrument. The resulting image quality allows seeing-limited performance down to seeing of 0.3 arcseconds FWHM. We also observed that our optical system produces a negative field curvature, which compensates the field curvature of the Ritchey-Chretien GTC design once the instrument is on the telescope.
    Proc SPIE 09/2012;
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    ABSTRACT: The Observatorio Astrofísico de Javalambre (OAJ) is a new astronomical facility located at the Sierra de Javalambre (Teruel, Spain) whose primary role will be to conduct all-sky astronomical surveys. The OAJ facility will have two wide-field telescopes: the JST/T250; a 2.55-m telescope with a 3° diameter field of view (FoV), and the JAST/T80; an 0.83-m telescope with a 2° diameter FoV. First light instrumentation is being designed to exploit the survey capabilities of the OAJ telescopes. This paper describes the T80Cam, a wide-field camera that will be installed at the Cassegrain focus of the JAST/T80. It is equipped with an STA 1600 backside illuminated detector. This is a 10.5k-by-10.5k, 9μm pixel, high efficiency CCD that is read from 16 ports simultaneously, allowing read times of ~20s with a typical read noise of 6 electrons (rms). This full wafer CCD covers a large fraction of the JAST/T80's FoV with a pixel scale of ~0.50"/pixel. T80Cam will observe in the wavelength range 330-1000nm through a set of 12 carefully optimized broad-, intermediate- and narrow-band filters. The camera is intended for surveys with the JAST/T80 telescope, starting with the planned J-PLUS (Javalambre Photometric Local Universe Survey), a multi-band photometric all-sky survey that will be completed in about 2 years and will reach AB˜ 23 mag (5σ level) with the SDSS filters.
    Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series; 09/2012
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    ABSTRACT: The Observatorio Astrofsico de Javalambre in Spain is a new astronomical facility particularly conceived for carrying out large sky surveys with two unprecedented telescopes of unusually large elds of view: the JST/T250, a 2.55m telescope of 3deg eld of view, and the JAST/T80, an 83cm telescope of 2deg eld of view. The most immediate objective of the two telescopes for the next years is carrying out two unique photometric surveys of several thousands square degrees, J-PAS and J-PLUS, each of them with a wide range of scientic applications, like e.g. large structure cosmology and Dark Energy, galaxy evolution, supernovae, Milky Way structure, exoplanets, among many others. To do that, JST and JAST will be equipped with panoramic cameras under development within the J-PAS collaboration, JPCam and T80Cam respectively, which make use of large format (~10k×10k) CCDs covering the entire focal plane. This paper describes the current status and expected schedule of the overall project, the main characteristics of the telescopes, their cameras, the technical requirements of the two planned surveys, as well as the general operation strategy of the observatory.
    Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series; 09/2012
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    ABSTRACT: J-PAS survey is going to observe 8000 deg2 in 54 optical narrow band filters plus 3 broad band ones. The survey will produce 1.2 PB of raw data in six years of observations. The treatment of about 1.5 TB per night, coming from the 14 detectors of the JPCam camera in the JST/T250, plus one detector in the JAST/T80 camera, shall be performed during the day after the operations. This contribution presents the software and hardware architecture designed to process and validate the data. The processing of the images is divided in two main stages. The first one, which deals with instrumental correction and data validation, is run daily. The second stage is run when a tile is completed and do the combination of the individual corrected frames and weight maps. To perform the astrometric calibration, image coadding and source extraction the data management pipeline uses software from the community which is integrated through Python. The software uses a database to control the process by storing the operations performed, parameters used and quality checks. This allows fast reprocessing to retrieve intermediate stages of the treatment from the raw data for any data release. This approach saves disk space by avoiding the storage of the processed individual frames. The data archiving and processing will be done in a data center 30 km away from the observatory. It will be equipped with ~2.5 PB of storage capacity to store the raw data and the final mosaics of the 57 filters, and processing power to deal with the incoming data.
    Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series; 09/2012
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    ABSTRACT: J-PAS survey consists of an 8000 square degree photometric sky survey with a set of 54 narrow-band, 2 mediumband and 1 broad-band filters. The main goal is to produce a photo-redshift catalog of 15 millions red, earlytype galaxies with a precision (z) 0:003(1 + z) to measure the Baryonic Acoustic Oscillation (BAO). Such precision requires specific care in the photometric calibration survey. This contribution presents the calibration protocol developed at CEFCA for the J-PAS data and to be applied from its first day. An auxiliary telescope JAST/T80 will perform an initial survey, J-PLUS, available before J-PAS, to create a set of flux calibrated stars in all J-PAS fields. Seven reference stars were already chosen to calibrate in flux the J-PLUS survey. J-PLUS 12-filter system was also specifically optimized to retrieve stellar parameters, T, log(g), [Fe/H], through the fitting of flux calibrated models. J-PLUS will be used as the standard network of flux calibrated stars to create synthetic spectro-photometry for J-PAS 56-filter system and to achieve the 1% photometric precision required for BAO measurements.
    Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series; 09/2012

Publication Stats

504 Citations
146.60 Total Impact Points

Institutions

  • 2013
    • Centro de Estudios de Física del Cosmos de Aragón
      Terol, Aragon, Spain
    • Dartmouth College
      • Department of Physics & Astronomy
      Hanover, New Hampshire, United States
  • 2010
    • Universidad de La Laguna
      • Department of Astrophysics
      San Cristóbal de La Laguna, Canary Islands, Spain
  • 2001–2010
    • Instituto de Astrofísica de Canarias
      San Cristóbal de La Laguna, Canary Islands, Spain
  • 2004–2007
    • University of Florida
      • Department of Astronomy
      Gainesville, Florida, United States