Stars, interstellar medium, galaxies, and the chemistry between them - A celebration to the outstanding career of Ángeles Díaz
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Stars, interstellar medium,
galaxies, and the chemistry
between them
A celebration to the
outstanding career of
Ángeles Díaz
Descubriendo el mundo de la
espectroscopia 2D junto a un Ángel
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...
Ángeles’ areas of expertice...
1. Starbursts
(some of!)
2. Ionizing stellar populations
3. Chemical evolution of galaxies
4. IR CaII triplet
5. Evolutionary synthesis models
6. Detailed spectroscopic studies of HII regions / galaxies
7. Chemical abundances in spiral discs
8. N/O evolution in galaxies
9. Circumnuclear star-forming regions
10. Precision abundance analysis of HII regions / galaxies
11. Photoionization models
12. Wolf-Rayet stars
13. Nucleosynthesis and primordial abundances
14. Nebular abundances based on the sulphur emission lines
15. Integral field spectroscopy
16. Spatially resolved chemical abundances
17. etc., etc.
Evolutionary phenomena in galaxies, Cambridge University Press, Cambridge and New York, 1989
Astrophysics and Space Science, 1998
Fructífera colaboración...
The path to wide-field
nebular emission studies
★ Multi-object instruments
e.g. Roy & Walsh 1998, Kennicutt & Garnett
1996, Moustakas & Kennicutt 2006
★ Narrow band imaging
e.g. Scowen et al 1996
★ Orion nebula survey
Sánchez et al 2007
★ HII galaxy II Zw 70
Kherig et al 2008
★ M33 Metallicity Project
Rosolowsky & Simon 2008
~ 1000 HII regions (multi-slit) The composition gradient in M101
Kennicutt & Garnet 1996
★ SAURON (2001)
72 E-type galaxies
z < 0.01 (large projected sizes)
The path to wide-field
nebular emission studies
★ Multi-object instruments
e.g. Roy & Walsh 1998, Kennicutt & Garnett
1996, Moustakas & Kennicutt 2006
★ Narrow band imaging
e.g. Scowen et al 1996
★ Orion nebula survey
Sánchez et al 2007
✦ Limited FoV
★ HII galaxy II Zw 70 ✦ Spectral coverage
Kherig et al 2008 ✦ Time expensive
✦ Complex data reduction
★ M33 Metallicity Project
Rosolowsky & Simon 2008
~ 1000 HII regions (multi-slit)
★ SAURON (2001)
72 E-type galaxies
z < 0.01 (large projected sizes)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)
IFU observed area ~ 80 arcmin2
Rosales-Ortega PhD Cantab 2009
Rosales-Ortega et al. 2010
✦ PMAS/PPAK instrument at CAHA
✦ Continuous coverage spectra: λ3700-7000 Å
✦ All bright lines for chemical empirical
calibrations: [OII] λ3727 - [SII] λλ6717,31and then CALIFA came...
Hα emission
Gas
velocity
SP Age
V-band
fluxThesis topics
• 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
Noviembre 2008Side Projects
• Diffuse interstellar gas • Local age dating vs.
extinction/reddening
• Integrated spectra
using Spitzer/GALEX/Hershel/optical
total/HII region/DIG
• SED maps
• SNRs/AGN
• Dust heating models
• Effects of co-adding spectra
for Av • Extinction models
• Kinematics • Spitzer vs. Optical
• Av(Ha/Hb) vs. IR/Ha • Ne abundances
vs. IR/UV
• Excitation/Ionization
Noviembre 2008The true nature of the
metallicity gradient of
NGC 1058
A. I. Díaz (UAM), R. C. Kennicutt (IoA, Cambridge), S. F. Sánchez (CAHA,IAA)
ESTALLIDOSNGC 1058
★ Type Sc
★ Projected size: 3.0 x 2.8 arcmin2
★ Distance: 10.6 Mpc
★ Perseus
Prolific host of SNe:
SN 1961V
SN 1969L
SN 2007gr
e.g. Li et al. 2007, Valenti et al. 2008NGC 1058
★ Type Sc
★ Projected size: 3.0 x 2.8 arcmin2
★ Distance: 10.6 Mpc
★ Perseus
Prolific host of SNe:
SN 1961V
SN 1969L
SN 2007gr
e.g. Li et al. 2007, Valenti et al. 2008
The Extreme Outer Regions of Disk Galaxies
Ferguson, Gallager & Wise, 1998R25
Rosales-Ortega PhD 2009
Rosales-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 7 dithered pointings covering the optical radius
✴ All bright lines for chemical +
empirical calibrations:
2 offsets ~ 2.5 arcmin north-east
[OII] λ3727 - [SII] λλ6717,31IFS-based HII regions catalogue
Rosales-Ortega PhD 2009NGC 1058: IFS-based oxygen abundance gradient
Calibration: Kobulnicky & Kewley 2004 Calibration: O3N2 Pettini & Pagel 2004
a) scale b) slope c) shapeSo, 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.
★ Alternative strong-line indicators: Sulphur !
Sulphur as abundance tracer in gaseous
nebulae
★ Sulphur is produced in massive stars, i.e.
“present day abundance”
returned to the ISM in a short time scale
★ Its yield is supposed to follow that of oxygen log(S/O) = -1.36
★ Provides similar information as oxygen,
abundance gradients!
despite being lees abundantAdvantages of the use of Sulphur as abundance tracer
Díaz & Pérez-Montero 2000, Pérez-Montero & Díaz 2005, Kehrig et al. 2006, Hägele et al. 2008, etc.
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
Empirical method
★ S is less abundant than O and emits at longer λ, i.e. its relevance as cooling agent starts
at lower temperatures (higher abundance)
log O/H log S/H
R23 S23WHT-ISIS programme to obtain a
Sulphur-based gradient of NGC 1058
5
★ Instrument: ISIS double arm spectrograph
★ Setup:
Blue arm R300B (λc 4400) + Red arm
4 R158B (λc 7800) + 5700 Dichroic
★ Spectral range: 3500 - 10000 Å
6 ★ Slit: 1.0 arcsec
3 1 ★ Emission lines coverage:
[OII] 3727 - [SIII] 9069, 9532 Å
2 ★ Six slit positions to optimise the coverage
of the galaxy disc
Ferguson, Gallager & Wise, 1998Region: FGW 1058E or PINGS N1058-58
ρ/ρ25 = 1.05
ISIS spectrum
Blue arm Red arm
[SIII] 9069, 9532 Å
WavelengthRegion: FGW 1058E or PINGS N1058-58
O3N2 Sulphur
FGW 1998 FGW PINGS ISIS ISIS
8.48 (empirical)
8.6
12 + log(O/H)
8.33
8.5 8.36
8.30
8.4
8.60
8.3
8.2
kappa effects?
Rosales-Ortega & Díaz in prep.Miralles-Caballero et al. in preparation
The effects of spatial resolution on Integral Field Unit Surveys
at different redshifts. The CALIFA perspective
Mast, Rosales-Ortega et al. 2013
V-band
Texto
PINGS: z ~ 0 CALIFA: z ~ 0.02 z ~ 0.05
HαThe effects of spatial resolution on Integral Field Unit Surveys
at different redshifts. The CALIFA perspective
Mast, Rosales-Ortega et al. 2013
V-band
abundance gradient
Texto
PINGS: z ~ 0 CALIFA: z ~ 0.02 z ~ 0.05
HαThe effects of spatial resolution in IFS
The effects of spatial resolution in IFS
NGC2906
CALIFAThe effects of spatial resolution in IFS
NGC2906
MUSE
CALIFAThe effects of spatial resolution in IFS
NGC2906
MUSE
CALIFA
Castellanos-Durán et al. in prep.Beyond MOS and fibers: large FoV Imaging Fourier Transform Spectroscopy
an instrumentation proposal for the present and future Mexican telescopes
IFTS-INAOEBeyond MOS and fibers: large FoV Imaging Fourier Transform Spectroscopy
an instrumentation proposal for the present and future Mexican telescopes
IFTS-INAOESELGIFS: Study of Emission Line Galaxies with
Integral Field Spectroscopy
Call
FP7 - PEOPLE - 2013 - IRSES
Funding scheme
Marie Curie Actions
International Research Staff Exchange Scheme (IRSES)Work Packages
1. New tools for the analysis of IFS data 2. Dimensional analysis
• Software & Algorithms • Mathematical characterisation
• Automatic separation of nebular and stellar • 2D chemical evolution models
spectra • Combination with multi-wavelength
• Reconstruction of the 2D SFH including data
kinematical information
3. Instrumentation 4. Training and dissemination
• Application to future IFS surveys • Software (publicly available)
• Extension to IR IFS data • Training (Summer schools)
• Visibility and outreachEl status....
• 2D spectroscopy is now a standard
technique in astronomy. Credits: R. García Benito, F. Rosales-Ortega, S. F. Sánchez,
E. Pérez, J. Walcher & the CALIFA team
• 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.
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 worldMuchas
Gracias
Ángeles!
Felicidades!You can also read
