Resolved stellar populations in the local Volume: the impact of JWST - - PowerPoint PPT Presentation

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Resolved stellar populations in the local Volume: the impact of JWST - - PowerPoint PPT Presentation

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Resolved stellar populations in the local Volume: the impact of JWST Supervisors: Alessandra Aloisi Roeland van der Marel Close collaborators: Elena Sacchi , postdoc @ Space Telescope Science Institute Michele Cignoni (UniPi) Understanding the

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Elena Sacchi, postdoc @ Space Telescope Science Institute Understanding the Nearby Star-forming Universe with JWST Courmayeur, August 30th, 2019

Resolved stellar populations in the local Volume: the impact of JWST

Supervisors:

Alessandra Aloisi Roeland van der Marel

Close collaborators:

Michele Cignoni (UniPi) Monica Tosi (INAF – OAS) & the LEGUS team

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SLIDE 2

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

How far we can go with HST

30 Mpc

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SLIDE 3

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST d

61 kpc 795 kpc 3.4 Mpc 18 Mpc Inner SMC (ACS) Cignoni+2012 Leo A (ACS) Cole+2007 NGC 1569 (ACS) Grocholski+2008 I Zw 18 (ACS) Aloisi+2007

The effect of distance

Elena Sacchi (esacchi@stsci.edu)

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SLIDE 4

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST

Why beyond the Local Group

Elena Sacchi (esacchi@stsci.edu)

Morphological variety Star Formation in action Environmental effects

NGC 1705 Blue Compact Dwarf NGC 4449 Magellanic Irregular Holmberg II Dwarf Irregular

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SLIDE 5

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST

Star Formation History and Color–Magnitude Diagram

Elena Sacchi (esacchi@stsci.edu)

Tolstoy + 2009 1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.0000 0.0001 0.0002 0.0003 0.0004 0.0005 0.0006 0.0007 SFR [M / yr]

constant SFH

1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.0000 0.0001 0.0002 0.0003 0.0004 0.0005 0.0006 0.0007 SFR [M / yr]

constant + recent burst

1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.00000 0.00001 0.00002 0.00003 0.00004 0.00005 0.00006 0.00007 0.00008 SFR [M / yr]

single old burst

1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.00000 0.00001 0.00002 0.00003 0.00004 0.00005 0.00006 0.00007 0.00008 SFR [M / yr]

two old bursts

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SLIDE 6

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST

Star Formation History and Color–Magnitude Diagram

Elena Sacchi (esacchi@stsci.edu)

Tolstoy + 2009 1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.0000 0.0001 0.0002 0.0003 0.0004 0.0005 0.0006 0.0007 SFR [M / yr]

constant SFH

1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.0000 0.0001 0.0002 0.0003 0.0004 0.0005 0.0006 0.0007 SFR [M / yr]

constant + recent burst

1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.00000 0.00001 0.00002 0.00003 0.00004 0.00005 0.00006 0.00007 0.00008 SFR [M / yr]

single old burst

1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.00000 0.00001 0.00002 0.00003 0.00004 0.00005 0.00006 0.00007 0.00008 SFR [M / yr]

two old bursts

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SLIDE 7

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST

Star Formation History and Color–Magnitude Diagram

Elena Sacchi (esacchi@stsci.edu)

Tolstoy + 2009 1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.0000 0.0001 0.0002 0.0003 0.0004 0.0005 0.0006 0.0007 SFR [M / yr]

constant SFH

1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.0000 0.0001 0.0002 0.0003 0.0004 0.0005 0.0006 0.0007 SFR [M / yr]

constant + recent burst

1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.00000 0.00001 0.00002 0.00003 0.00004 0.00005 0.00006 0.00007 0.00008 SFR [M / yr]

single old burst

1 2 3 4 5 6 7 8 9 10 11 12 13 Lookback Time [Gyr] 0.00000 0.00001 0.00002 0.00003 0.00004 0.00005 0.00006 0.00007 0.00008 SFR [M / yr]

two old bursts

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SLIDE 8

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

Observational

¡1 1 2 3 4 5 mF555W ¡ mF814W 18 19 20 21 22 23 24 25 26 27 mF814W

NGC 4449

The synthetic CMD method

[Tosi+1991] LEGUS survey [Calzetti+2015, Sabbi+2018, Sacchi+2018]

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SLIDE 9

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

Observational Theoretical

¡1 1 2 3 4 5 mF555W ¡ mF814W 18 19 20 21 22 23 24 25 26 27 mF814W ¡1 1 2 3 4 5 mF555W ¡ mF814W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 mF814W 1 Myr 5 Myr 10 Myr 20 Myr 50 Myr 100 Myr 200 Myr 500 Myr 1 Gyr 5 Gyr 10 Gyr

MESA/MIST isochrones waps.cfa.harvard.edu/MIST

NGC 4449 Z = 0.0015

The synthetic CMD method

[Tosi+1991] LEGUS survey [Calzetti+2015, Sabbi+2018, Sacchi+2018]

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SLIDE 10

¡1 1 2 3 4 5 mF555W ¡ mF814W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 mF814W 1 Myr 5 Myr 10 Myr 20 Myr 50 Myr 100 Myr 200 Myr 500 Myr 1 Gyr 5 Gyr 10 Gyr

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

Observational Theoretical

¡1 1 2 3 4 5 mF555W ¡ mF814W 18 19 20 21 22 23 24 25 26 27 mF814W

NGC 4449 Z = 0.0015

IMF binary fraction

The synthetic CMD method

[Tosi+1991]

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SLIDE 11

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

Observational Theoretical

¡1 1 2 3 4 5 mF555W ¡ mF814W 18 19 20 21 22 23 24 25 26 27 mF814W

NGC 4449

¡1 1 2 3 4 5 mF555W ¡ mF814W 18 19 20 21 22 23 24 25 26 27 mF814W

distance incompleteness photometric errors

The synthetic CMD method

[Tosi+1991] differential reddening

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SLIDE 12

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

Observational Theoretical

¡1 1 2 3 4 5 mF555W ¡ mF814W 18 19 20 21 22 23 24 25 26 27 mF814W

NGC 4449

¡1 1 2 3 4 5 mF555W ¡ mF814W 18 19 20 21 22 23 24 25 26 27 mF814W Z = 0:0046 Z = 0:0015 Z = 0:0005

The synthetic CMD method

[Tosi+1991]

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SLIDE 13

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

Observational Theoretical

¡1 1 2 3 4 5 mF555W ¡ mF814W 18 19 20 21 22 23 24 25 26 27 mF814W ¡1 1 2 3 4 5 mF555W ¡ mF814W 18 19 20 21 22 23 24 25 26 27 mF814W Z = 0:0046 Z = 0:0015 Z = 0:0005

N(i) = wZ,t ×CMDZ,t

t

∑

(i)

Z

∑

The synthetic CMD method

[Tosi+1991]

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SLIDE 14

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST

Star Formation Evolution Recovery Algorithm

[Cignoni+2015]

INPUT parameters:

  • stellar tracks/isochrones
  • initial mass function
  • binary fraction
  • metallicity range

Monte Carlo extractions

  • f (mass, age) pairs

Convolution with:

  • distance
  • extinction
  • photometric errors
  • incompleteness

ASTs synthetic CMDs DATA

minimization

  • f the

residuals hybrid genetic algorithm Poissonian approach

χ P =

  • i ln oi

mi

i=1 Nbin

∑

−oi + mi

Elena Sacchi (esacchi@stsci.edu)

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SLIDE 15

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

From the data

  • photometric depth
  • photometric errors
  • incompleteness
  • Poisson noise
  • dust obscuration
  • differential reddening

SFH derivation – all kinds of uncertainties From the method

  • CMD binning
  • SF/Z steps
  • assumed parameters

(e.g. IMF, binary fraction, distance, extinction law)

From the models

  • mass loss
  • core convective overshooting
  • stellar rotation
  • TP-AGB phase modeling
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SLIDE 16

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

SFH derivation – all kinds of uncertainties

1 2 3 4 F555W-F814W

  • 8
  • 7
  • 6
  • 5
  • 4
  • 3
  • 2
  • 1

F814W 1e8 5e8 1e9 5e9 1 2 3 4 F555W-F814W

  • 8
  • 7
  • 6
  • 5
  • 4
  • 3
  • 2
  • 1

F814W 1e8 5e8 1e9 5e9

PARSEC/COLIBRI 2017 PARSEC/COLIBRI 2018

1 2 3 4 F555W-F814W

  • 8
  • 7
  • 6
  • 5
  • 4
  • 3
  • 2
  • 1

F814W 1e8 5e8 1e9 5e9

MESA/MIST 2018

¡1 1 2 3 4 5 mF555W ¡ mF814W 18 19 20 21 22 23 24 25 26 27 mF814W

From the models

  • mass loss
  • core convective overshooting
  • stellar rotation
  • TP-AGB phase modeling
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SLIDE 17

Volume surveyed in 10, 100, and 1000 hours reaching 0.5 mag below the turnoff of a 12 Gyr

  • ld stellar population

[Brown+2008]

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST

From HST to JWST: the gain in sensitivity

Elena Sacchi (esacchi@stsci.edu)

HST resolution + much larger aperture

nearby surveys will be ∼6 times faster deep surveys will reach galaxies 50% further away

=>

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SLIDE 18

¡0:5 0:5 1:0 1:5 2:0 2:5 mF090W ¡ mF200W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF200W ¡0:5 0:5 1:0 1:5 2:0 2:5 mF606W ¡ mF814W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF814W

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

From HST to JWST

MESA/MIST isochrones ACS/WFC filters [Fe/H] = –2.0 MESA/MIST isochrones NIRCam filters [Fe/H] = –2.0

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SLIDE 19

¡0:5 0:5 1:0 1:5 2:0 2:5 mF090W ¡ mF200W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF200W ¡0:5 0:5 1:0 1:5 2:0 2:5 mF606W ¡ mF814W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF814W

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

From HST to JWST: the gain in age resolution higher color separations more accurate age measurements =>

MESA/MIST isochrones ACS/WFC filters [Fe/H] = –2.0 MESA/MIST isochrones NIRCam filters [Fe/H] = –2.0

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SLIDE 20

¡0:5 0:5 1:0 1:5 2:0 2:5 mF090W ¡ mF200W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF200W ¡0:5 0:5 1:0 1:5 2:0 2:5 mF606W ¡ mF814W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF814W

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

From HST to JWST: unveiling fainter stellar phases

  • TP–AGB: near–mid IR ideal for dusty envelopes
  • RGB Tip: more than 1 mag brighter => better distances
  • Red Clump: ∼1 mag brighter => better ages in the range 1–10 Gyr
  • Red Horizontal Branch: ∼1 mag brighter => probably visible up to 4 Mpc

MESA/MIST isochrones ACS/WFC filters [Fe/H] = –2.0 MESA/MIST isochrones NIRCam filters [Fe/H] = –2.0

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SLIDE 21

¡0:5 0:5 1:0 1:5 2:0 2:5 mF090W ¡ mF200W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF200W ¡0:5 0:5 1:0 1:5 2:0 2:5 mF606W ¡ mF814W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF814W

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

  • TP–AGB: near–mid IR ideal for dusty envelopes
  • RGB Tip: more than 1 mag brighter => better distances
  • Red Clump: ∼1 mag brighter => better ages in the range 1–10 Gyr
  • Red Horizontal Branch: ∼1 mag brighter => probably visible up to 4 Mpc

MESA/MIST isochrones ACS/WFC filters [Fe/H] = –2.0 MESA/MIST isochrones NIRCam filters [Fe/H] = –2.0

From HST to JWST: unveiling fainter stellar phases

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SLIDE 22

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

  • TP–AGB: near–mid IR ideal for dusty envelopes
  • RGB Tip: more than 1 mag brighter => better distances
  • Red Clump: ∼1 mag brighter => better ages in the range 1–10 Gyr
  • Red Horizontal Branch: ∼1 mag brighter => probably visible up to 4 Mpc

¡0:5 0:5 1:0 1:5 2:0 2:5 mF090W ¡ mF200W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF200W ¡0:5 0:5 1:0 1:5 2:0 2:5 mF606W ¡ mF814W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF814W

MESA/MIST isochrones ACS/WFC filters [Fe/H] = –2.0 MESA/MIST isochrones NIRCam filters [Fe/H] = –2.0

From HST to JWST: unveiling fainter stellar phases

slide-23
SLIDE 23

¡0:5 0:5 1:0 1:5 2:0 2:5 mF090W ¡ mF200W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF200W ¡0:5 0:5 1:0 1:5 2:0 2:5 mF606W ¡ mF814W ¡10 ¡9 ¡8 ¡7 ¡6 ¡5 ¡4 ¡3 ¡2 ¡1 1 mF814W

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

  • TP–AGB: near–mid IR ideal for dusty envelopes
  • RGB Tip: more than 1 mag brighter => better distances
  • Red Clump: ∼1 mag brighter => better ages in the range 1–10 Gyr
  • Red Horizontal Branch: ∼1 mag brighter => probably visible up to 4 Mpc

MESA/MIST isochrones ACS/WFC filters [Fe/H] = –2.0 MESA/MIST isochrones NIRCam filters [Fe/H] = –2.0

From HST to JWST: unveiling fainter stellar phases

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SLIDE 24

Resolved stellar populations in the local Volume: the impact of JWST

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

Summary Although not specifically designed for photometric studies in the local Universe, JWST will provide many new insights into resolved stellar population science, allowing to expand the current knowledge on Star Formation Histories beyond the Local Group [see, e.g., Cignoni+2018,2019(submitted), Sacchi+2016,2018,2019, McQuinn+2010,2012, Weisz+2011]. The capabilities of NIRCam will be very relevant in:

  • pushing the limits of CMD analysis of external galaxies
  • allowing faster and deeper surveys of the local Volume
  • providing more accurate age measurements
  • unveiling fainter stellar phases such as
  • dust obscured TP–AGB stars
  • RGB Tip stars
  • Red Clump stars
  • Horizontal Branch stars
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SLIDE 25

Understanding the Nearby Star-forming Universe with JWST Elena Sacchi (esacchi@stsci.edu)

THE LOCAL GROUP

Assembly and Evolution

Annalisa Calamida (chair) Elena Sacchi (chair) Tony Sohn (chair) Tom Brown Carol Christian Andres del Pino Karoline Gilbert

SOC

STScI Spring Symposium:
 20-24 April, 2020

Claus Leitherer Mattia Libralato Nora Luetzgendorf Peter Zeidler Erik Tollerud Rosemary Wyse Mike Boylan-Kolchin

  • How did the Milky Way system assemble and form?
  • How similar/different are the MW and M31?
  • What mechanisms are involved in the formation and

evolution of the LG and its galaxies?

  • What are the differences between the LG and other groups

in the local universe?

TOPICS