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

The local neighbourhood

Roberto Muñoz2 Mpc

Going beyond

Roberto Muñoz60 Mpc

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

DECam @ 4m BlancoThere 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

DECam @ 4m BlancoThere 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

DES surveyDES 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

DES surveyDES 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

DES survey Y2

Roberto Muñoz

12 TB

DES survey Y2

Roberto Muñoz

8 new ultra-faint dwarf galaxies Drlica-Wagner et al. 2015

12 TB

NGFS: Fornax clusterThe 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

45

6

7

10

1330 deg2

NGFS: Fornax clusterThe 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

45

6

7

10

1330 deg2

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

The Neighbourhood Watch Survey

Roberto Muñoz

The Neighbourhood Watch Survey

Roberto Muñoz60 Mpc

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

NGFS central tile

Roberto Muñoz

NGFS central tile

Roberto Muñoz

NGFS central tile

Roberto Muñoz

Non-nucleated dwarfs - bright

Roberto Muñoz

Mi = �16.6µi = 21.8

Mi = �13.4µi = 24.5

Non-nucleated dwarfs - faint

Roberto Muñoz

Mi = �9.31µi = 25.2

Mi = �8.0µi = 27.9

Size-Luminosity relation

Roberto Muñoz

Muñoz et al., 2015

Spatial distribution

Roberto Muñoz

Eigenthaler et al., in prep.Muñoz et al. 2015

Data reduction and analysisWe 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 Muñozwww.github.com/rpmunoz

SummaryThe 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