SAGES Legacy Unifying Globulars and GalaxieS Survey

Colour thumbnails of the 25 galaxies in the SLUGGS survey.

Project

The SLUGGS (SAGES Legacy Unifying Globulars and GalaxieS) survey is an astronomical survey of 25 nearby early-type (E and S0) galaxies. This survey uses a combination of imaging from Subaru/Suprime-Cam and spectroscopy from Keck/DEIMOS to investigate the chemo-dynamical properties of both the diffuse starlight and the globular cluster systems of the target galaxies. Pilot data for the survey was obtained in 2006 and data acquisition is going to be completed in 2015.^[1]

Method

Deep wide-field imaging from Subaru/Suprime-Cam is used to identify and measure the positions of candidate globular clusters around each survey galaxy. Several (up to 4) DEIMOS masks are then created which include slits corresponding to the locations of globular clusters, galaxy starlight and random background sky locations in the outer parts of the mask. The DEIMOS spectrograph is centred on wavelengths around the Calcium Triplet lines (~850 nm). After a typical 2 hour exposure per mask, spectra of globular clusters and galaxy starlight is obtained. Using a technique called SKiMS (Stellar Kinematics from Multiple Slits) it is possible to extract the kinematics (and metallicity) of galaxy starlight out to 3 effective radii. Equivalent data for the globular clusters is obtained out to ~10 effective radii. The DEIMOS instrument has the advantages of being a stable, high throughput, wide-field spectrograph coupled with excellent velocity resolution (~12 km/s) on a 10m telescope. This technique effectively uses DEIMOS as a pseudo wide area integral field unit.^[2]

Survey selection

The 25 target galaxies are chosen to be representative (i.e. cover the range of basic galaxy parameters and environments) of nearby (distance < 27 Mpc) early type (E and S0) galaxies. The survey also includes 3 `bonus’ galaxies which have been observed during times that the main sample galaxies are not available. All galaxies are accessible from the northern hemisphere. Although only a small sample, the data reach to large galactocentric radii with excellent velocity resolution and S/N compared to other surveys.^[3]

Key science questions

1. What are the basic, global chemo-dynamical properties of early type galaxies?
2. What is the distribution of dark matter in early-type galaxies?
3. How are the outer regions of early-type galaxies assembled?
4. How does assembly depend on mass, environment, and other variables?
5. Do the observations agree with theoretical models of galaxy formation?

Target galaxies

NGC 720, NGC 821, NGC 1023, NGC 1400, NGC 1407, NGC 2768, NGC 2974, NGC 3115, NGC 3377, NGC 3608, NGC 4111, NGC 4278, NGC 4365, NGC 4374, NGC 4459, NGC 4473, NGC 4474, NGC 4486, NGC 4494, NGC 4526, NGC 4564, NGC 4649, NGC 4697, NGC 5846, NGC 7457.

The bonus galaxies are NGC 3607, NGC 4594 and NGC 5866.

Further reading

• "The SAGES Legacy Unifying Globulars and GalaxieS Survey (SLUGGS): Sample Definition, Methods, and Initial Results"; J. P. Brodie et al., 2014, ApJ, 796, 52 link;
• "The SLUGGS Survey: Wide-field Stellar Kinematics of Early-type Galaxies"; J. Arnold et al., 2014, ApJ, 791, 80 link;
• "The SLUGGS Survey: exploring the metallicity gradients of nearby early-type galaxies to large radii"; N. Pastorello et al., 2014, MNRAS, 442, 1003 link;
• "The SLUGGS Survey: kinematics for over 2500 globular clusters in 12 early-type galaxies"; V. Pota et al., 2013, MNRAS, 428, 389 link;
• "The SLUGGS Survey: calcium triplet-based spectroscopic metallicities for over 900 globular clusters"; C. Usher et al., 2012, MNRAS, 426, 1475 link;
• "The SLUGGS survey: inferring the formation epochs of metal-poor and metal-rich globular clusters"; D. A. Forbes et al., 2015, MNRAS, 452, 1045 link;

Notes

A complete list of publications using SLUGGS survey data can be found here.

References

External links

• SLUGGS survey official website: http://sluggs.swin.edu.au/