PMAS: The Potsdam Multi‐Aperture Spectrophotometer. II. The Wide Integral Field Unit PPak

By A. Kelz, Marc A. W. Verheijen, M. Roth, S. Bauer, T. Becker, J. Paschke, E. Popow, S. Sánchez, U. Laux. 2005

195 citations recorded by the source corpus.

PPak is a new fiber‐based integral field unit (IFU) developed at the Astrophysical Institute of Potsdam and implemented as a module into the existing Potsdam Multi‐Aperture Spectrophotometer (PMAS) spectrograph. The purpose of PPak is to provide an extended field of view with a large light‐collecting power for each spatial element, as well as an adequate spectral resolution. The PPak system consists of a fiber bundle with 331 object fibers, 36 sky fibers, and 15 calibration fibers. The object and sky fibers collect the light from the focal plane behind a focal reducer lens. The object fibers of PPak, each 2 .″7 in diameter, provide a contiguous hexagonal field of view of 74″ × 64″ on the sky, with a filling factor of 60%. The operational wavelength range is from 400 to 900 nm. The PPak IFU, together with the PMAS spectrograph, are intended for the study of extended, low surface brightness objects, offering an optimization of total light‐collecting power and spectral resolution. This paper describes the instrument design, the assembly, integration, and tests, the commissioning and operational procedures, and presents the measured performance at the telescope.

Subfields: Atomic and Molecular Physics, and Optics, Biomedical Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/0d8c746cea65d4dac35ac780ef66910b481bc1a1

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Citations in the corpus

CALIFA, the Calar Alto Legacy Integral Field Area survey - III. Second public data release (2012, methodology): “…started in June 2010 with the Potsdam Multi Aperture Spectrograph (PMAS, Roth et al. 2005), mounted to the 3.5 m telescope, utilizing the large (74 (cid:48)(cid:48) × 64 (cid:48)(cid:48) ) hexagonal ﬁeld-of-view (FoV) o ﬀ ered by the PPak ﬁber bundle (Verheijen et al. 2004; Kelz et al. 2006).”
THE DISKMASS SURVEY. I. OVERVIEW (2010, background): “SparsePak (Bershady et al. 2004, 2005) and PPak (Verheijen et al. 2004, Kelz et al. 2006) are large-fiber IFUs on – 11 – 3.5m telescopes (WIYN3 and Calar Alto, respectively) with fields-of-view of slightly over 1 arcminute.”
CALIFA : a diameter-selected sample for an integral field spectroscopy galaxy survey (2014, methodology): “The instrument used for CALIFA is the Potsdam Multi-Aperture Spectrophotometer (PMAS, Roth et al. 2005) mounted on the 3.5 m telescope of the Calar Alto observatory, and employing the PPak wide-field integral field unit (IFU, Kelz et al. 2006) to sample a field of view (FoV) of ∼1 arcmin2.”
Mass-metallicity relation explored with CALIFA I. Is there a dependence on the star-formation rate? (2013, methodology): “All galaxies were observed using PMAS (Roth et al. 2005) in the PPAK configuration (Kelz et al. 2006), covering a hexagonal field-ofview of 74′′×64′′, sufficient to cover the full optical extent of the galaxies up to 2-3 effective radii.”
A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA (2013, methodology): “All galaxies were observed using PMAS (Roth et al. 2005) in the PPAK configuration (Kelz et al. 2006), covering a hexagonal field-of-view (FoV) of 74′′×64′′, sufficient to map the full optical extent of the galaxies up to two to three disk effective radii.”
Metallicity gradients in local field star-forming galaxies: insights on inflows, outflows, and the coevolution of gas, stars and metals (2015, methodology): “Every CALIFA galaxy is observed using the fibre bundle integral field unit (IFU) PPak, and two different setups with the Potsdam Multi-Aperture Spectrophotometer (PMAS;Roth et al. 2005; Kelz et al. 2006).”
OVERVIEW OF THE SDSS-IV MaNGA SURVEY: MAPPING NEARBY GALAXIES AT APACHE POINT OBSERVATORY (2014, methodology): “…power of the CALIFA, SAMI, and MaNGA survey instrumentation, displayed as a function of wavel ngth. Relevant to both metrics is the total system efficiency ( ) which is adopted from the literature for CALIFA (Roth et al. 2004; Kelz et al. 2006; Sánchez et al. 2012) and SAMI (Bryant et al. 2014).”
The DiskMass Survey VII. The distribution of luminous and dark matter in spiral galaxies (2013, methodology): “In this paper, we decompose the rotation curves of 30 spiral galaxies, using stellar kinematics from PPak (Verheijen et al. 2004; Kelz et al. 2006) and ionized gas kinematics from SparsePak (Bershady et al. 2004, 2005), as well as 21-cm radio synthesis data from the WSRT, GMRT and VLA,…”
The star formation history of CALIFA galaxies: Radial structures (2013, unknown): “′′ diameter each, covering a 74′′ × 64′′ Field of View (FoV, Kelz et al. 2006).”
THE MANGA INTEGRAL FIELD UNIT FIBER FEED SYSTEM FOR THE SLOAN 2.5 M TELESCOPE (2014, methodology): “This can be mitigated (e.g., Kelz et al. 2006) by including sacrificial edge fibers, acting as stress buffers for the live fibers in the interior of the IFU.”
The CALIFA survey across the Hubble sequence: Spatially resolved stellar population properties in galaxies (2015, unknown): “PPaK contains 382 fibers of 2.7′′ diameter each, and a 74′′ × 64′′ Field of View (FoV Kelz et al. 2006).”