Pucón Symposium 2015 Puerto Varas, Agosto 2015

Chasing ghost galaxies in the Fornax clusterOpportunities for the Deep Learning

community

Paul Eigenthaler, Thomas Puzia, 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

Galaxy clustersGravitationally bound structures that contain from hundreds to thousands of galaxies. They are dominated by dark matter (85%) and have large amounts of hot gas (10%). Why so interesting? • Large amount of galaxies at the same distance • Laboratories to study the influence of

environment • Rare objects formed from the most overdense

peaks in the initial density field

Coma is the best studied cluster • Distance of 100 Mpc • More than 1,000 members • Mass of about

Roberto Muñoz

2⇥ 1015 M�

Diffuse galaxies in Comavan Dokkum et al. (2015) published a paper with 47 new dwarf galaxies. A couple are diffuse galaxies, sizes similar to the Milky Way but much fainter.

Roberto Muñoz

Virgo and Fornax clustersVirgo 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)

4 Murakami et al. [Vol. ,

Fig. 1. (left) Suzaku-XIS (0.5–4.0 keV) image of the Fornax cluster. The NXB was subtracted and the difference in exposuretimes was corrected. The Cosmic X-ray background (CXB) was not subtracted. (middle) Raw XMM-MOS image (0.8–1.2 keV)of the Fornax cluster. Magenta circles correspond to field of view of the XMM observations. Red squares indicate the four offsetobservations with Suzaku. Blue pie and black square regions summarize the accumulation area of spectral analysis. (right) Exposure-and vignetting-corrected and adaptively smoothed XMM-MOS image (0.8–1.2 keV). The NXB and CXB were not subtracted.

Table 1. Suzaku and XMM observations of the Fornax cluster and background fields

Fields Seq. No. (R.A., Dec.) in J2000.0 Date of obs. Exp. time (after screenings)Suzaku observations of the Fornax clusterCenter 100020010 (3h38m35.s7, −35◦28′14.′′5) 2005/09/13 76 ksNorth 800002010 (3h38m51.s9, −35◦14′23.′′6) 2006/01/05 78 ksFar North 802021010 (3h38m55.s9, −34◦57′32.′′4) 2008/01/14 56 ksSouth 803006010 (3h38m19.s6, −35◦45′49.′′1) 2008/07/15 35 ksNorth West 803007010 (3h37m25.s7, −35◦16′52.′′7) 2008/07/16 41 ksNorth East 803008010 (3h40m07.s5, −35◦09′04.′′1) 2008/07/17 41 ksSuzaku observations of the Fornax Galactic fieldGalactic1 802037010 (3h13m11.s0, −37◦40′48.′′0) 2007/06/28 20 ksGalactic2 802040010 (3h19m57.s7, −32◦04′18.′′8) 2007/06/29 21 ksXMM observations of the Fornax cluster MOS1, MOS2, PNA 0550930101 (3h39m02s.4, -35◦01′55′′.2) 2008/06/28 10.6, 11.2, 7.0 ksB 0550930201 (3h39m26s.2, -34◦49′37′′.2) 2008/06/27 7.6, 6.7, 3.5 ksC 0550930301 (3h40m27s.1, -34◦59′16′′.8) 2008/07/17 11.4, 11.6, 8.0 ksD 0550930401 (3h41m25s.0, -35◦10′04′′.8) 2009/02/09 14.5, 15.1, 11.7 ksE 0550930501 (3h41m40s.8, -35◦22′51′′.6) 2009/02/23 18.1, 17.8, 14.6 ksF 0550930601 (3h41m35s.0, -35◦37′48′′.0) 2009/02/24 17.7, 17.9, 13.7 ksG 0550930701 (3h40m52s.1, -35◦50′02′′.4) 2009/02/24 0, 0, 0 ksJ 0550931001 (3h37m38s.9, -35◦45′18′′.0) 2008/06/25 19.1, 19.4, 11.7ksL 0550931201 (3h36m15s.6, -35◦32′56′′.4) 2008/06/25 0, 0, 0 ksN 0550931401 (3h37m11s.5, -35◦17′34′′.8) 2008/06/26 11.0, 11.4, 8.0 ksNGC 1399 0400620101 (3h38m29s.1, -35◦27′03′′.0) 2006/08/23 99.6, 102.7, 53.2 ksNGC 1404 0304940101 (3h38m51s.9, -35◦35′39′′.8) 2005/07/30 24.6, 15.0, 17.0 ksLP 944-20 0055140101 (3h39m34s.60, -35◦25′51′′.0) 2001/01/07 43.0, 43.2, 36.5 ksRXJ 0337-3457 0210480101 (3h37m24s.70, -34◦57′29′′.0) 2005/01/04 44.3, 44.4, 37.9 ksNGC 1386 0140950201 (3h36m45s.4, -35◦59′57′′.0) 2002/12/29 15.9, 15.9, 12.8 ks

Fornax cluster in X-ray from XMM.(Murakami et al 2011)

Virgo and Fornax clustersVirgo 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)

4 Murakami et al. [Vol. ,

Fig. 1. (left) Suzaku-XIS (0.5–4.0 keV) image of the Fornax cluster. The NXB was subtracted and the difference in exposuretimes was corrected. The Cosmic X-ray background (CXB) was not subtracted. (middle) Raw XMM-MOS image (0.8–1.2 keV)of the Fornax cluster. Magenta circles correspond to field of view of the XMM observations. Red squares indicate the four offsetobservations with Suzaku. Blue pie and black square regions summarize the accumulation area of spectral analysis. (right) Exposure-and vignetting-corrected and adaptively smoothed XMM-MOS image (0.8–1.2 keV). The NXB and CXB were not subtracted.

Table 1. Suzaku and XMM observations of the Fornax cluster and background fields

Fields Seq. No. (R.A., Dec.) in J2000.0 Date of obs. Exp. time (after screenings)Suzaku observations of the Fornax clusterCenter 100020010 (3h38m35.s7, −35◦28′14.′′5) 2005/09/13 76 ksNorth 800002010 (3h38m51.s9, −35◦14′23.′′6) 2006/01/05 78 ksFar North 802021010 (3h38m55.s9, −34◦57′32.′′4) 2008/01/14 56 ksSouth 803006010 (3h38m19.s6, −35◦45′49.′′1) 2008/07/15 35 ksNorth West 803007010 (3h37m25.s7, −35◦16′52.′′7) 2008/07/16 41 ksNorth East 803008010 (3h40m07.s5, −35◦09′04.′′1) 2008/07/17 41 ksSuzaku observations of the Fornax Galactic fieldGalactic1 802037010 (3h13m11.s0, −37◦40′48.′′0) 2007/06/28 20 ksGalactic2 802040010 (3h19m57.s7, −32◦04′18.′′8) 2007/06/29 21 ksXMM observations of the Fornax cluster MOS1, MOS2, PNA 0550930101 (3h39m02s.4, -35◦01′55′′.2) 2008/06/28 10.6, 11.2, 7.0 ksB 0550930201 (3h39m26s.2, -34◦49′37′′.2) 2008/06/27 7.6, 6.7, 3.5 ksC 0550930301 (3h40m27s.1, -34◦59′16′′.8) 2008/07/17 11.4, 11.6, 8.0 ksD 0550930401 (3h41m25s.0, -35◦10′04′′.8) 2009/02/09 14.5, 15.1, 11.7 ksE 0550930501 (3h41m40s.8, -35◦22′51′′.6) 2009/02/23 18.1, 17.8, 14.6 ksF 0550930601 (3h41m35s.0, -35◦37′48′′.0) 2009/02/24 17.7, 17.9, 13.7 ksG 0550930701 (3h40m52s.1, -35◦50′02′′.4) 2009/02/24 0, 0, 0 ksJ 0550931001 (3h37m38s.9, -35◦45′18′′.0) 2008/06/25 19.1, 19.4, 11.7ksL 0550931201 (3h36m15s.6, -35◦32′56′′.4) 2008/06/25 0, 0, 0 ksN 0550931401 (3h37m11s.5, -35◦17′34′′.8) 2008/06/26 11.0, 11.4, 8.0 ksNGC 1399 0400620101 (3h38m29s.1, -35◦27′03′′.0) 2006/08/23 99.6, 102.7, 53.2 ksNGC 1404 0304940101 (3h38m51s.9, -35◦35′39′′.8) 2005/07/30 24.6, 15.0, 17.0 ksLP 944-20 0055140101 (3h39m34s.60, -35◦25′51′′.0) 2001/01/07 43.0, 43.2, 36.5 ksRXJ 0337-3457 0210480101 (3h37m24s.70, -34◦57′29′′.0) 2005/01/04 44.3, 44.4, 37.9 ksNGC 1386 0140950201 (3h36m45s.4, -35◦59′57′′.0) 2002/12/29 15.9, 15.9, 12.8 ks

Fornax cluster in X-ray from XMM.(Murakami et al 2011)

Ferrarese et al. 2012

The uiK diagram

Roberto Muñoz

Muñoz et al. 2014

Ferrarese et al. 2012

Globular clusters

The improved uiK diagram

Roberto Muñoz

Powalka et al., in preparation

NGFS: Fornax clusterThe Next Generation Fornax Survey (NGFS; PI: R. Muñoz) is an ongoing multipassband optical and NIR survey of the Fornax galaxy cluster. It will cover the central 30 deg2 out to the virial radius and will allow to study the GC and galaxy populations.

Roberto Muñoz

8 deg

Globular clusters

Galaxies

Observations and ProcessingThere 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/DECam

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Observations and ProcessingThere 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/DECam

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Observations and ProcessingThere 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/DECam

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Observations and ProcessingThere 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/DECam

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Observations and ProcessingThere 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/DECam

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45

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Observations and ProcessingThere 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/DECam

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2

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45

6

7

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Observations and ProcessingThere 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/DECam

1

2

3

45

6

7

10

13

Observations and ProcessingThere 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/DECam

1

2

3

45

6

7

10

13

Observations and ProcessingThere 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/DECam

1

2

3

45

6

7

10

13

Observations and ProcessingThere 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/DECam

1

2

3

45

6

7

10

13

Observations and Processing

Roberto Muñoz

Raw

CP detrended NGFS pipeline

Registration and stacking

Roberto Muñoz

Registration and stacking

Roberto Muñoz

Exposure=300s

Registration and stacking

Roberto Muñoz

Exposure=300s Exposure=17x300s = 1.5 hours

Registration and stacking

Roberto Muñoz

Exposure=300s Exposure=17x300s = 1.5 hours

Dwarf galaxies

Color image asinhThe survey is still ongoing, but we already have deep u, g and i-band for several tiles.

Roberto Muñoz

Muñoz et al., 2015

Color image asinhThe survey is still ongoing, but we already have deep u, g and i-band for several tiles.

Roberto Muñoz

Muñoz et al., 2015

Color image asinhThe survey is still ongoing, but we already have deep u, g and i-band for several tiles.

Roberto Muñoz

Muñoz et al., 2015

Dwarfs galaxiesWe have discovered 200 new dwarf galaxies just in the central 3 deg2 of the Fornax cluster. Still 27 deg2 more to explore.

Roberto Muñoz

Muñoz, Eigenthaler, Puzia, Taylor et al., 2015

Equivalent to IGM between Milky Way and Andromeda (~780 kpc)

Milky Way

Andromeda

•~70 deg2

•u’g’r’i’z’ •~3σ past GCLF turnover •~26-27 mag/arcsec^2

•spatial extent of Centaurus A’s ~300 kpc virial radius

*optical

SCABS: A Survey of Centaurus A’s Baryonic Structures

SCABS: A Survey of Centaurus A’s Baryonic Structures

Taylor et al., in preparation

SummaryThe NGFS survey is a multi wavelength optical and NIR survey of the Fornax cluster. We have developed new algorithms and methods for doing image processing of DECam data. Special focus on modelling the spatial variations of the sky. We have done visual classification of the central tile and it’s exhausting. We have discovered 200 new dwarf galaxies just in the central DECam tile. We need to invite the community to help us with the identification. There are opportunities for the researchers working in deep learning to develop methods to automatise the identification of dwarf galaxies.

Roberto Muñoz