MEGARA, the new intermediate-resolution optical IFU and MOS for GTC: getting ready for the telescope

Paz, A. Gil de; Carrasco, E.; Gallego, J.; Iglésias-Páramo, J.; Cedazo, R.; Vargas, M.; Arrillaga, X.; Avilés, Javier; Cardiel, N.; Carrera, M. A.; Castillo-Morales, A.; Castillo‐Domínguez, E.; Garcı́a, J.; Román, Segundo Esteban San; Ferrusca, D.; Gómez-Álvarez, P.; Izazaga-Pérez, Rafael; Lefort, Bertrand; López-Orozco, J. A.; Maldonado, Manuel; Martínez-Delgado, I.; Durán, I.; Mujica, E.; Паез, Гонзало; Pascual, S.; Pérez-Calpena, A.; Picazo-Sanchez, Pablo; Sánchez-Penim, A.; Sánchez-Blanco, E.; Tulloch, Simon; Velázquez, Miguel; Vı́lchez, J. M.; Zamorano, J.; Aguerri, Alfonso L.; Barrado, D.; Bertone, E.; Cava, A.; Cenarro, J.; Chávez, M.; García, M. A.; García‐Rojas, J.; Guichard, J.; Delgado, R. M. González; Guzmán, R.; Herrero, A.; Huélamo, N.; Hughes, D. H.; Jiménez-Vicente, J.; Kehrig, C.; Marino, R. A.; Márquez, I.; Masegosa, J.; Mayya, Y. D.; Méndez-Abreu, J.; Mollá, M.; Muñoz–Tuñón, C.; Peimbert, M.; Pérez‐González, P. G.; Montero, E. Pérez; Rodriguez, Mario; Rodríguez-Espinosa, J. M.; Rodríguez-Merino, L. H.; Rodríguez-Muñoz, L.; Rosa-González, D.; Sánchez-Almeida, J.; Contreras, C. Sánchez; Sánchez‐Blázquez, P.; Moreno, Francisco Miguel; Sanchez, S. F.; Sarajedini, Ata; Silich, Sergiy; Tenorio-Tagle, G.; Terlevich, Elena; Terlevich, R.; Torres-Peimbert, S.; Trujillo, Ignacio; Tsamis, Y. G.; Vega, O.

doi:10.1117/12.2231988

Cited by 13 publications

(6 citation statements)

References 23 publications

(43 reference statements)

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“…In addition, for this particular aim, the CALIFA spectral resolution is at the limit of what is needed to perform such multicomponent kinematical fitting. Future highefficiency IFS facilities working at R > 5000, such as MEGARA (at GTC; Gil de Paz et al 2016) or WEAVE (at WHT; Dalton et al 2014), will help in that regard.…”

Section: Assigning Sfr Values To Morphological Componentsmentioning

confidence: 99%

Star Formation in the Local Universe from the CALIFA Sample. II. Activation and Quenching Mechanisms in Bulges, Bars, and Disks

Catalán-Torrecilla

Paz

Castillo-Morales

et al. 2017

ApJ

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We estimate the current extinction-corrected Hα star formation rate (SFR) of the different morphological components that shape galaxies (bulges, bars, and disks). We use a multicomponent photometric decomposition based on Sloan Digital Sky Survey imaging to Calar Alto Legacy Integral Field Area Integral Field Spectroscopy (IFS) datacubes for a sample of 219 galaxies. This analysis reveals an enhancement of the central SFR and specific SFR (sSFR=SFR/M å ) in barred galaxies. Along the main sequence, we find that more massive galaxies in total have undergone efficient suppression (quenching) of their star formation, in agreement with many studies. We discover that more massive disks have had their star formation quenched as well. We evaluate which mechanisms might be responsible for this quenching process. The presence of type 2 AGNs plays a role at damping the sSFR in bulges and less efficiently in disks. Also, the decrease in the sSFR of the disk component becomes more noticeable for stellar masses around  M 10 ; 10.5 for bulges, it is already present at~ M 10 9.5 . The analysis of the line-of-sight stellar velocity dispersions (σ) for the bulge component and of the corresponding Faber-Jackson relation shows that AGNs tend to have slightly higher σ values than star-forming galaxies for the same mass. Finally, the impact of environment is evaluated by means of the projected galaxy density, Σ 5 . We find that the SFR of both bulges and disks decreases in intermediate-to high-density environments. This work reflects the potential of combining IFS data with 2D multicomponent decompositions to shed light on the processes that regulate the SFR.

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Section: Assigning Sfr Values To Morphological Componentsmentioning

confidence: 99%

Star Formation in the Local Universe from the CALIFA Sample. II. Activation and Quenching Mechanisms in Bulges, Bars, and Disks

Catalán-Torrecilla

Paz

Castillo-Morales

et al. 2017

ApJ

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“…Category (1) includes the study of Galactic Planetary Nebulae, nearby galaxies, and the high-redshift IGM while in category (2) we find Galactic open stellar clusters, resolved stellar populations in Local Group galaxies, intermediateredshift dwarf and starburst galaxies, and high-redshift cluster galaxies (see Figure 2). More details on the science drivers of the MEGARA instrument have been published elsewhere 1,2,3,4,5 . Some of these scientific goals are now pursued using either Open Time (2018B observations started on July 1 st 2018) or Guaranteed Time observations.…”

Section: Science Driversmentioning

confidence: 99%

MEGARA, the R=6000-20000 IFU and MOS of GTC

Carrasco

Paz

Gallego

et al. 2018

Ground-Based and Airborne Instrumentation for Astronomy VII

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MEGARA is the new generation IFU and MOS optical spectrograph built for the 10.4m Gran Telescopio CANARIAS (GTC). The project was developed by a consortium led by UCM (Spain) that also includes INAOE (Mexico), IAA-CSIC (Spain) and UPM (Spain). The instrument arrived to GTC on March 28 th 2017 and was successfully integrated and commissioned at the telescope from May to August 2017. During the on-sky commissioning we demonstrated that MEGARA is a powerful and robust instrument that provides on-sky intermediate-to-high spectral resolutions R FWHM ~ 6,000, 12,000 and 20,000 at an unprecedented efficiency for these resolving powers in both its IFU and MOS modes. The IFU covers 12.5 x 11.3 arcsec 2 while the MOS mode allows observing up to 92 objects in a region of 3.5 x 3.5 arcmin 2. In this paper we describe the instrument main subsystems, including the Folded-Cassegrain unit, the fiber link, the spectrograph, the cryostat, the detector and the control subsystems, and its performance numbers obtained during commissioning where the fulfillment of the instrument requirements is demonstrated.

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“…Both modes are fed by 100 μm fiber core. The IFU provides a FOV of 12.5″ × 11.3″, while the MOS shall be able to place up to 100 mini-bundles with 7 fibers each (100 μm fibercore) covering a sky area of 3.5 × 3.5 arcmin 2 . The science light will come into the spectrograph from one of the Folded Cassegrain focus (where the LCB and MOS subsystems are located and telecentrically illuminated with the aims of a field lens), by means of a 44.5 m fiber optic wiring.…”

Section: Introductionmentioning

confidence: 99%

MEGARA: high-precision alignment system for gluing fibers and microlenses

et al. 2016

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MEGARA is the multi-object medium-resolution spectrograph for the GTC 10m telescope. MEGARA offers two observing modes, the LCB mode, a large central IFU; and a MOS mode composed by 92 robotic positioners carrying 7 fibers minibundles. Microlens are required to fit the GTC f/17 to the f/3 at the fiber entrance, where pupil image is oversized to have a fiber-to-fiber flux variation better than 10%. This tight requirement imposed manufacturing tolerances for the different components and required the development of a gluing station to provide a centering precision better than 5μm. We present the overview of the optical bundles, the gluing station and the final performance obtained during the integration and tests.

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MEGARA, the new intermediate-resolution optical IFU and MOS for GTC: getting ready for the telescope

Cited by 13 publications

References 23 publications

Star Formation in the Local Universe from the CALIFA Sample. II. Activation and Quenching Mechanisms in Bulges, Bars, and Disks

Star Formation in the Local Universe from the CALIFA Sample. II. Activation and Quenching Mechanisms in Bulges, Bars, and Disks

MEGARA, the R=6000-20000 IFU and MOS of GTC

MEGARA: high-precision alignment system for gluing fibers and microlenses

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