Ma pping N earby G alaxies at A pache Point Observatory Bruno - - PowerPoint PPT Presentation

Mapping Nearby Galaxies at Apache Point Observatory

Bruno Rodríguez Del Pino CAB (INTA-CSIC)

Main MaNGA papers:

• General Overview (Bundy et al. 2015)
• Data Reduction Pipeline (Law et al. 2016)
• Observation strategy (Law et al. 2015)
• IFU Instrument description (Drory et al. 2015)

Integral Field Spectroscopy of ~10 000 nearby galaxies

MaNGA is one of the three core programs of SDSS-IV, with eBOSS and APOGEE-2

MaNGA general overview

From SDSS to MaNGA

• Spectral resolution:


R~1400 at 4000Å (90km/s) to R ~2600 at 9000Å (49km/s)

• Wavelength coverage: 


360-1000 nm

• Multiplexed: 17 IFU per plate
• IFU bundle sizes: 19, 37, 61, 91, 127
• Fiber size: 2” on the sky (1-2 kpc)
• Spatial PSF ~2.5 arcsec

calibration bundle

(standard stars)

~32 arcsec ~12 arcsec +~100 sky fibres

MaNGA general overview

• Sample size: wide and uniform coverage in

stellar mass, color and density.

• Sample selection:
• Flat stellar mass distribution (M*≥109 Msun)
• Uniform radial coverage based on Re.
• S/N: at least 5 per Å in continuum at 1.5Re

ar& !

ieband!absolute!magnitude!(Mi)!

Primary sample (~5000): 1.5Re for >80% of its targets (<z> = 0.03) + “Color-Enhanced sample” (~1700): including high-mass blue galaxies, low-mass red ones and “green valley” objects). ~6700 Secondary sample (~3300): 2.5Re for >80% of its targets (<z> = 0.045) Ancillary targets outside main sample: ~10%

6 bins per parameter 50 galaxies per bin } 63 x 50 = 10 800

MaNGA general overview

étendue: How quickly one can map the sky to a given S/N at a given R

Comparison with other IFU surveys

Bundy et al. 2015

MaNGA is the only survey mapping galaxy clusters

Bundy et al. 2015

IC0674

SDSS image Hα map (QFitsView) Hα map (QFitsView)

SDSS DR13 - MaNGA DR1 (Aug. 2016)

1 390 galaxies (1351 unique objects) 600 in the Primary Sample

+ 216 in the “Color Enhanced”

473 in the Secondary Sample 62 extra galaxies, some of them ancillary

TABLE 3 Summary of MaNGA Ancillary Programs with Data in DR13 Ancillary Program Number of Targets

1

BITNAME binary digit value Luminous AGN 1 AGN BAT 1 2 4 AGN OIII 2 4 Edge-On Star-forming Galaxies 4 EDGE ON WINDS 6 64 Close Pairs and Mergers 5 PAIR ENLARGE 7 128 10 PAIR RECENTER 8 256 1 PAIR SIM 9 512 1 PAIR 2IFU 10 1024 Massive Nearby Galaxies 1 MASSIVE 12 4096 Milky Way Analogs 2 MWA 13 8192 Dwarf Galaxies in MaNGA 2 DWARF 14 16384 Brightest Cluster Galaxies 2 BCG 17 131072 MaNGA Resolved Stellar Populations 1 ANGST 18 262144

1 An individual galaxy can be targeted by more than one ancillary program.

SDSS DR13 - MaNGA DR1 (Aug. 2016)

largest public sample of galaxies with IFU spectroscopy

What comes with DR13?

Data:

• Raw Data (before Data Reduction Pipeline)
• Raw Stacked Spectra (RSS): row-stacked, flux-calibrated

fiber spectra for a given galaxy across all exposures

• Reduced data cubes, rearranged in a regular 0.5” grid.

Catalogues:

• ‘drpall’ (v1_5_4 for DR13) main table containing:
• plateifu: identifies an observation
• mangaid: identifies an object for a given catalogue
• RA, DEC, redshift, data quality, etc., of all objects
• No higher-level science products, scheduled for DR14 (July 2017)

SDSS DR13 - MaNGA DR1 (Aug. 2016)

What DOES NOT comes with DR13?

SDSS DR13 - MaNGA DR1 (Aug. 2016)

Online information available

Tutorials:

• How to interact with the ‘drpall’ file.
• How to download MaNGA data.
• How to open and visualise data cubes.

Data models: containing all the information about the ‘drpall’ catalog, raw data, RSS data and data cubes. Targeting catalogue: Primary, secondary, ancillary… MaNGA Field Layout Forecast and whether a galaxy will be observed in MaNGA Ancillary targets and programs MaNGA caveats

• Reconstructed PSF FWHM is 2.5 arcsec
• Spectral resolution is overestimated by ~10% (also appeared in SDSS

data). It is planned to be fixed in future releases.

• Data cube covariance (from the redistribution of light) not included:

when combining spectra from multiple spaxels the noise has to be calibrated (see Law et al. 2016). More details on: http://www.sdss.org/dr13/manga/manga-caveats/ and DR13 paper

Caveats

Caveats

http://www.sdss.org/dr13/manga/manga-caveats/

http://www.sdss.org/dr13/manga/manga-data/data-access/

Data Acces

http://www.sdss.org/dr13/manga/manga-tutorials/how-do-i-look-at-my-data/

Data Acces

8138-12705

Data Acces

EXT0 (PRIMARY): Main header EXT1 (FLUX): 3d rectified cube in units of 10^{-17} erg/s/cm2/Å/spaxel EXT2 (IVAR): Inverse variance cube EXT3 (MASK): Pixel mask cube EXT4 (WAVE): Wavelength vector in units of Angstroms EXT5 (SPECRES): Median (among fibers) resolution vs lambda EXT6 (SPECRESD): Standard deviation (1σ) of spectral resolution vs lambda EXT7 (OBSINFO): Table describing exposures combined to create this file EXT8,9,10,11: Broadband SDSS g,r,i,z images created from the data cube EXT12,13,14,15: Reconstructed SDSS g,r,i,z point source response profile

Content of a single data cube

Data Acces

Bulge-Disc Decomposition of IFU Datacubes (BUDDI) Johnston et al. 2016

Done with MaNGA data

MaNGA Survey

• largest IFU survey up to date. It will contain ~10 000 galaxies

by 2020.

• Large spectral coverage and spatial up to 2.5 Re.
• Uniform and wide sampling in stellar mass, color and

environment. MaNGA DR1

• SDSS DR13 contains ~1400 objects already reduced.
• Lots of information and help available online.
• One per year until 2020 when all data will be released

Future Data Releases Conclusions

MaNGA Survey

• largest IFU survey up to date. It will contain ~10 000 galaxies

by 2020.

• Large spectral coverage and spatial up to 2.5 Re.
• Uniform and wide sampling in stellar mass, color and

environment. MaNGA DR1

• SDSS DR13 contains ~1400 objects already reduced.
• Lots of information and help available online.
• One per year until 2020 when all data will be released

Future Data Releases Conclusions