Astronomy in the Data Driven Science Era
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The document discusses the Next Generation Fornax Survey (NGFS), an ongoing multi-wavelength survey of the Fornax galaxy cluster. The goal of the NGFS is to produce a photometric catalog of globular clusters, ultra compact dwarfs, giant galaxies, and dwarf galaxies in Fornax. The detection and analysis of dwarf galaxies from the survey data is challenging. So far, dwarf galaxies have been detected in two survey tiles by visual inspection, but automated methods are being tested. Developing efficient data reduction and analysis pipelines is important for analyzing dwarf galaxies from the deep survey images.
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Astronomy in the Data Driven Science Era
- 1. 2nd PUC-OSU Workshop Santiago, May 2016 Chasing ghost galaxies in the Fornax cluster: Living in the Data-Driven Science Era Thomas Puzia, Paul Eigenthaler, Matt Taylor, Yasna Ordenes, Simón Angel, Maren Hempel Ariane Lançon, Steffen Mieske, Michael Hilker, Patrick Côté, Laura Ferrarese & NGFS team. Roberto Muñoz Instituto de Astrofísica Pontificia Universidad Católica de Chile
- 2. The local neighbourhood Roberto Muñoz2 Mpc
- 3. Going beyond Roberto Muñoz60 Mpc
- 4. Virgo and Fornax clusters Virgo is the largest nearby galaxy cluster. It contains about 1,762 members (Binggeli et al. 1985) and is located at 16.5 Mpc Fornax is the second closest cluster. It contains about 340 members (Ferguson et al. 1989) and is located at 20.0 Mpc. Roberto Muñoz Virgo cluster in X-ray from ROSAT (Böhringer et al. 1994) Murakami et al. [Vol. , –4.0 keV) image of the Fornax cluster. The NXB was subtracted and the difference in exposure Fornax cluster in X-ray from XMM. (Murakami et al 2011)
- 5. Virgo and Fornax clusters Virgo is the largest nearby galaxy cluster. It contains about 1,762 members (Binggeli et al. 1985) and is located at 16.5 Mpc Fornax is the second closest cluster. It contains about 340 members (Ferguson et al. 1989) and is located at 20.0 Mpc. Roberto Muñoz Virgo cluster in X-ray from ROSAT (Böhringer et al. 1994) Murakami et al. [Vol. , –4.0 keV) image of the Fornax cluster. The NXB was subtracted and the difference in exposure Fornax cluster in X-ray from XMM. (Murakami et al 2011) Ferrarese et al. 2012
- 6. The uiK diagram Roberto Muñoz Muñoz et al. 2014 Ferrarese et al. 2012 Globular clusters
- 7. DECam @ 4m Blanco There is no universal observational strategy neither universal image processing pipeline. It all depends on the scientific goals of the project and the instrument been used. Roberto Muñoz CTIO 4m telescope DECam 60 CCDs 3 deg2
- 8. DECam @ 4m Blanco There is no universal observational strategy neither universal image processing pipeline. It all depends on the scientific goals of the project and the instrument been used. Roberto Muñoz CTIO 4m telescope DECam 60 CCDs 3 deg2
- 9. DES survey DES is an ongoing optical imaging survey of 5,000 deg2 in the South Galactic cap using DECam. It consists of griYz bands photometry. DES was scheduled for 525 nights over 5 years. Roberto Muñoz 26 TB
- 10. DES survey DES is an ongoing optical imaging survey of 5,000 deg2 in the South Galactic cap using DECam. It consists of griYz bands photometry. DES was scheduled for 525 nights over 5 years. Roberto Muñoz 9 new ultra-faint dwarf galaxies Koposov et al. 2015 Drlica-Wagner et al. 2015 26 TB
- 11. DES survey Y2 Roberto Muñoz 12 TB
- 12. DES survey Y2 Roberto Muñoz 8 new ultra-faint dwarf galaxies Drlica-Wagner et al. 2015 12 TB
- 13. NGFS: Fornax cluster The Next Generation Fornax Survey (NGFS; PI: R. Muñoz) is an ongoing multi-wavelength optical and NIR survey of the Fornax galaxy cluster. It will cover the central 30 deg2 out to the virial radius Study GCs, UCDs and galaxies. Roberto Muñoz 1.8 Mpc Globular clusters Galaxies 1 2 3 4 5 6 7 10 13 30 deg2
- 14. NGFS: Fornax cluster The Next Generation Fornax Survey (NGFS; PI: R. Muñoz) is an ongoing multi-wavelength optical and NIR survey of the Fornax galaxy cluster. It will cover the central 30 deg2 out to the virial radius Study GCs, UCDs and galaxies. Roberto Muñoz 1.8 Mpc Globular clusters Galaxies 1 2 3 4 5 6 7 10 13 30 deg2
- 15. NGFS and beyond Roberto Muñoz 60 deg2 3.2 Mpc Andromeda 0.7 Mpc Muñoz et al., in prep Taylor et al., in prep Milky Way 60 deg2
- 16. The Neighbourhood Watch Survey Roberto Muñoz
- 17. The Neighbourhood Watch Survey Roberto Muñoz60 Mpc
- 18. Observations and Processing Roberto Muñoz Raw CP detrended NGFS pipeline
- 19. Registration and stacking Roberto Muñoz
- 20. Registration and stacking Roberto Muñoz Exposure=300s
- 21. Registration and stacking Roberto Muñoz Exposure=300s Exposure=17x300s = 1.5 hours
- 22. Registration and stacking Roberto Muñoz Exposure=300s Exposure=17x300s = 1.5 hours Dwarf galaxies
- 23. NGFS central tile Roberto Muñoz
- 24. NGFS central tile Roberto Muñoz
- 25. NGFS central tile Roberto Muñoz
- 26. Non-nucleated dwarfs - bright Roberto Muñoz Mi = 16.6 µi = 21.8 Mi = 13.4 µi = 24.5
- 27. Non-nucleated dwarfs - faint Roberto Muñoz Mi = 9.31 µi = 25.2 Mi = 8.0 µi = 27.9
- 28. Size-Luminosity relation Roberto Muñoz Muñoz et al., 2015
- 29. Spatial distribution Roberto Muñoz Eigenthaler et al., in prep. Muñoz et al. 2015
- 30. Data reduction and analysis We have been developing pipelines for Optical and NIR cameras. Most of the pipelines are in IDL and some have been ported to Python. Most of the codes are CPU based, but we are moving towards GPU image processing. We are modelling the sky by using Radial basis functions and Gaussian process regressions. Roberto Muñoz www.github.com/rpmunoz
- 31. Summary The NGFS survey is a multi wavelength optical and NIR survey of the Fornax cluster. The goal is producing a photometric catalog of GCs, UCDs, giant and dwarf galaxies in Fornax. The detection and analysis of dwarf galaxies is challenging. So far, we have detected dwarf galaxies in tiles 1 and 4 by doing visual inspection. We are testing several methods to automatise the process. Having access to good quality data reduction pipelines is very important. Measuring dwarf galaxies with was possible because of deep data and a good pipeline. Plenty of space for improvements in data reduction and analysis software. Limits are set by the people writing good quality and efficient software. Roberto Muñoz µi = 28 mag/arcsec2