The effects of spatial resolution on integral field spectrograph surveys at different redshifts - The CALIFA perspective

D. Mast, F. F. Rosales-Ortega, S. F. Sánchez, J. M. Vílchez, J. Iglesias-Paramo, C. J. Walcher, B. Husemann, I. Márquez, R. A. Marino, R. C. Kennicutt, A. Monreal-Ibero, L. Galbany, Adriana De Lorenzo-Caceres Rodriguez, Jairo Mendez Abreu, C. Kehrig, A. del Olmo, M. Relaño, L. Wisotzki, E. Mármol-Queraltó, S. BekeraitèP. Papaderos, V. Wild, J. A. L. Aguerri, J. Falcón-Barroso, D. J. Bomans, B. Ziegler, B. García-Lorenzo, J. Bland-Hawthorn, Á. R. López-Sánchez, G. van de Ven

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Abstract

Context. Over the past decade, 3D optical spectroscopy has become the preferred tool for understanding the properties of galaxies and is now increasingly used to carry out galaxy surveys. Low redshift surveys include SAURON, DiskMass, ATLAS3D, PINGS, and VENGA. At redshifts above0.7, surveys such as MASSIV, SINS, GLACE, and IMAGES have targeted the most luminous galaxies to study mainly their kinematic properties. The on-going CALIFA survey (z ~ 0.02) is the first of a series of upcoming integral field spectroscopy (IFS) surveys with large samples representative of the entire population of galaxies. Others include SAMIand MaNGA at lower redshift and the upcoming KMOS surveys at higher redshift. Given the importance of spatial scales in IFS surveys, the study of the effects of spatial resolution on the recovered parameters becomes important. Aims: We explore the capability of the CALIFA survey and a hypothetical higher redshift survey to reproduce the properties of a sample of objects observed with better spatial resolution at lower redshift. Methods: Using a sample of PINGS galaxies, we simulated observations at different redshifts. We then studied the behaviour of different parameters as the spatial resolution degrades with increasing redshift. Results: We show that at the CALIFA resolution, we are able to measure and map common observables ina galaxy study: the number and distribution of H ii regions (Hαflux structure), the gas metallicity (using the O3N2 method), the gas ionization properties (through the [N II]/Hα and [O III]/Hβline ratios), and the age of the underlying stellar population (using the D4000 index). This supports the aim of the survey to characterise the observable properties of galaxies in the Local Universe. Our analysis of simulated IFS data cubes at higher redshifts highlights the importance of the projected spatial scale per spaxel as the most important figure of merit in the design of an integral field survey.

Original languageEnglish
Article numberA129
Number of pages19
JournalAstronomy & Astrophysics
Volume561
Early online date22 Jan 2014
DOIs
Publication statusPublished - 22 Jan 2014

Keywords

  • Techniques: spectroscopic
  • Galaxies: abundances
  • Stars: formation
  • Galaxies: ISM
  • Galaxies: stellar content

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