stars, interstellar medium, galaxies, and the chemistry...

Descubriendo el mundo de la espectroscopia 2D junto a un Ángel

Stars, interstellar medium, galaxies, and the chemistry

between them

A celebration to the outstanding career of

Ángeles Díaz

F. Fabián Rosales Ortega

Mi trabajo con Ángeles...

‣ 2004-2005: first met @ INAOE

‣ 2006: on sabbatical @ IoA, Cambridge‣ my 1st PhD year @ IoA‣ collaboration begins

‣ 2006-2009: PhD programme‣ several stay visits to UAM

‣ 2011-2012: postdoc @ UAM

‣ since 2007: continuous collaboration...

1. Starbursts2. Ionizing stellar populations3. Chemical evolution of galaxies4. IR CaII triplet5. Evolutionary synthesis models6. Detailed spectroscopic studies of HII regions / galaxies7. Chemical abundances in spiral discs8. N/O evolution in galaxies9. Circumnuclear star-forming regions10. Precision abundance analysis of HII regions / galaxies11. Photoionization models12. Wolf-Rayet stars13. Nucleosynthesis and primordial abundances14. Nebular abundances based on the sulphur emission lines15. Integral field spectroscopy16. Spatially resolved chemical abundances17. etc., etc.

Ángeles’ areas of expertice...(some of!)

Evolutionary phenomena in galaxies, Cambridge University Press, Cambridge and New York, 1989

Astrophysics and Space Science, 1998

Fructífera colaboración...

The composition gradient in M101Kennicutt & Garnet 1996

The path to wide-field nebular emission studies

★ Multi-object instrumentse.g. Roy & Walsh 1998, Kennicutt & Garnett 1996, Moustakas & Kennicutt 2006

★ Narrow band imaginge.g. Scowen et al 1996

★ Orion nebula surveySánchez et al 2007

★ HII galaxy II Zw 70Kherig et al 2008

★ M33 Metallicity ProjectRosolowsky & Simon 2008

~ 1000 HII regions (multi-slit)

★ SAURON (2001)72 E-type galaxiesz < 0.01 (large projected sizes)

✦ Limited FoV✦ Spectral coverage✦ Time expensive✦ Complex data reduction

meter lo de VENGA

★ Multi-object instrumentse.g. Roy & Walsh 1998, Kennicutt & Garnett 1996, Moustakas & Kennicutt 2006

★ Narrow band imaginge.g. Scowen et al 1996

★ Orion nebula surveySánchez et al 2007

★ HII galaxy II Zw 70Kherig et al 2008

★ M33 Metallicity ProjectRosolowsky & Simon 2008

~ 1000 HII regions (multi-slit)

★ SAURON (2001)72 E-type galaxiesz < 0.01 (large projected sizes)

The path to wide-field nebular emission studies

La historia de un doctorado...

‣ 2006, 2º semestre

‣ IoA Cambridge: 8 semanas de cursos PhD

‣ supervisor? Robert C. Kennicutt ó Max Pettini

‣ Max en sabático...

‣ Rob, the Plumian Professor on Astrophysics!

‣ Propuesta 1: Spitzer data, extinction, dust heating, etc.

‣ Propuesta 2: SFR, GALEX data, IR connection, etc.

‣ Propuesta 3: ...

‣ Propuesta 4: “something that we’ve wanted to do since 20 years ago...”

‣ 2D spectroscopy (Ángeles!)

CAHA: Semester B - 2007

Wide-Field Integral Field Spectroscopy Survey of Nearby Galaxies (< 100 Mpc)

Rosales-Ortega PhD Cantab 2009Rosales-Ortega et al. 2010

IFU observed area ~ 80 arcmin2

✦ PMAS/PPAK instrument at CAHA

✦ Continuous coverage spectra: λ3700-7000 Å

✦ All bright lines for chemical empirical calibrations: [OII] λ3727 - [SII] λλ6717,31

and then CALIFA came...

V-band flux

SP Age

Gas velocity

Hα emission

• Z/Z⦿ vs. radius

• Residuals vs. L(Hα)• Residuals vs. Location• (Z/Z⦿)Te vs. Strong Lines

• WR / OB stars vs. Abundance• Error analysis simulations• Yields

Thesis topics

Noviembre 2008

• Diffuse interstellar gas

• Integrated spectra total/HII region/DIG

• SNRs/AGN

• Effects of co-adding spectra for Av

• Kinematics

• Av(Ha/Hb) vs. IR/Ha vs. IR/UV

• Excitation/Ionization

• Local age dating vs. extinction/reddeningusing Spitzer/GALEX/Hershel/optical

• SED maps

• Dust heating models

• Extinction models

• Spitzer vs. Optical

• Ne abundances

Side Projects

Noviembre 2008

A. I. Díaz (UAM), R. C. Kennicutt (IoA, Cambridge), S. F. Sánchez (CAHA,IAA)

ESTALLIDOS

The true nature of the metallicity gradient of

NGC 1058

NGC 1058★ Type Sc ★ Projected size: 3.0 x 2.8 arcmin2 ★ Distance: 10.6 Mpc★ Perseus

e.g. Li et al. 2007, Valenti et al. 2008

Prolific host of SNe:SN 1961VSN 1969LSN 2007gr

NGC 1058★ Type Sc ★ Projected size: 3.0 x 2.8 arcmin2 ★ Distance: 10.6 Mpc★ Perseus

Ferguson, Gallager & Wise, 1998

The Extreme Outer Regions of Disk Galaxies

e.g. Li et al. 2007, Valenti et al. 2008

Prolific host of SNe:SN 1961VSN 1969LSN 2007gr

Rosales-Ortega PhD 2009Rosales-Ortega et al. 2010

Wide-Field Integral Field Spectroscopy Survey of Nearby Galaxies

(< 100 Mpc)

✴ PMAS/PPAK instrument at CAHA✴ Spectral range: λ3700-7000 Å

✴ All bright lines for chemical empirical calibrations:

[OII] λ3727 - [SII] λλ6717,31

7 dithered pointings covering the optical radius+

2 offsets ~ 2.5 arcmin north-east

R25

IFS-based HII regions catalogueRosales-Ortega PhD 2009

NGC 1058: IFS-based oxygen abundance gradient

Calibration: Kobulnicky & Kewley 2004 Calibration: O3N2 Pettini & Pagel 2004

a) scale b) slope c) shape

So, what is the true nature of the abundance gradient in NGC 1058 ?

★ Methods using direct measurement of Te ?e.g. [OIII] λ4363, [SIII] λ6312, etc.

Sulphur as abundance tracer in gaseous nebulae

★ Sulphur is produced in massive stars, i.e. returned to the ISM in a short time scale

★ Its yield is supposed to follow that of oxygen

★ Provides similar information as oxygen, despite being lees abundant

“present day abundance”

log(S/O) = -1.36

abundance gradients!

★ Alternative strong-line indicators: Sulphur !

Advantages of the use of Sulphur as abundance tracer

Direct method

★ The NIR lines [SIII] 6312, 9069, 9532 are analogous to those of [OIII] 4363, 4959, 5007, but their emissivities are less dependent on Te

Díaz & Pérez-Montero 2000, Pérez-Montero & Díaz 2005, Kehrig et al. 2006, Hägele et al. 2008, etc.

★ S is less abundant than O and emits at longer λ, i.e. its relevance as cooling agent starts at lower temperatures (higher abundance)

Empirical method

R23

log O/H

S23

log S/H

WHT-ISIS programme to obtain a Sulphur-based gradient of NGC 1058

1

2

3

4

5

6

★ Instrument: ISIS double arm spectrograph

★ Setup:

Blue arm R300B (λc 4400) + Red arm

R158B (λc 7800) + 5700 Dichroic

★ Spectral range: 3500 - 10000 Å

★ Slit: 1.0 arcsec

★ Emission lines coverage:

[OII] 3727 - [SIII] 9069, 9532 Å

★ Six slit positions to optimise the coverage

of the galaxy disc

Ferguson, Gallager & Wise, 1998

Wavelength

Red arm

ISIS spectrum

Blue arm

Region: FGW 1058E or PINGS N1058-58

ρ/ρ25 = 1.05

[SIII] 9069, 9532 Å

FGW 1998 PINGS ISISFGW

O3N2 Sulphur12

+ lo

g(O

/H)

8.2

8.3

8.4

8.5

8.6

8.60

8.338.36

8.30

8.48

ISIS

(empirical)

Region: FGW 1058E or PINGS N1058-58

Rosales-Ortega & Díaz in prep.

kappa effects?

Miralles-Caballero et al. in preparation

Mast, Rosales-Ortega et al. 2013

The effects of spatial resolution on Integral Field Unit Surveys at different redshifts. The CALIFA perspective

PINGS: z ~ 0 CALIFA: z ~ 0.02 z ~ 0.05

Texto

V-band

Hα

Mast, Rosales-Ortega et al. 2013

The effects of spatial resolution on Integral Field Unit Surveys at different redshifts. The CALIFA perspective

PINGS: z ~ 0 CALIFA: z ~ 0.02 z ~ 0.05

Texto

V-band

Hα

abundance gradient

The effects of spatial resolution in IFS

CALIFA

NGC2906

The effects of spatial resolution in IFS

CALIFA

NGC2906

MUSE

The effects of spatial resolution in IFS

Castellanos-Durán et al. in prep.CALIFA

NGC2906

MUSE

The effects of spatial resolution in IFS

Beyond MOS and fibers: large FoV Imaging Fourier Transform Spectroscopyan instrumentation proposal for the present and future Mexican telescopes

IFTS-INAOE

Beyond MOS and fibers: large FoV Imaging Fourier Transform Spectroscopyan instrumentation proposal for the present and future Mexican telescopes

IFTS-INAOE

SELGIFS: Study of Emission Line Galaxies with Integral Field Spectroscopy

CallFP7 - PEOPLE - 2013 - IRSES

Funding schemeMarie Curie ActionsInternational Research Staff Exchange Scheme (IRSES)

Work Packages

1. New tools for the analysis of IFS data

• Software & Algorithms• Automatic separation of nebular and stellar

spectra• Reconstruction of the 2D SFH including

kinematical information

2. Dimensional analysis

• Mathematical characterisation• 2D chemical evolution models• Combination with multi-wavelength

data

3. Instrumentation

• Application to future IFS surveys• Extension to IR IFS data

4. Training and dissemination

• Software (publicly available)• Training (Summer schools)• Visibility and outreach

El status....• 2D spectroscopy is now a standard

technique in astronomy.

• IFS has flourished in large aperture, high resolution instruments. Technology is becoming mature.

• IFS has opened a new window in galaxy evolution research by passing to a 2D spectroscopic description.

Credits: R. García Benito, F. Rosales-Ortega, S. F. Sánchez, E. Pérez, J. Walcher & the CALIFA team

El futuro....• Spatially-resolved chemical evolution modelling

(Mercedes)

• Define a new paradigm in data analysis, methodologies, theoretical modelling and interpretation.

• SELGIFS

• New instrumentation (IFTS)

• Conquer the world

Muchas Gracias Ángeles!

Felicidades!