The ALMA-IMF continuum data

Adam Ginsburg, for the ALMA-IMF data reduction team:
Frédérique Motte, Adam Ginsburg, Patricio Sanhueza, Fabien Louvet, Sylvain Bontemps, Csengeri Timea, Roberto Galván-Madrid, Fumitaka Nakamura, Amelia Stutz, Thomas Nony, Ana Lopez-Sepulcre, Tapas Baug, Nichol Cunningham, Manuel Fernandez Lopez, Andres E Guzman, Liu Hongli, Luke Maud, Fernando Olguin, Yohan Pouteau, Allison Towner
And the consortium: Jonathan Braine, Edwige Chapillon, Huei-Ru Vivien Chen, Antoine Gusdorf, Natsuko Izumi, Xing (Walker) Lu, Jordan Molet, Brian Svoboda, K. Tatematsu, Rodrigo (Hernan) Alvarez (Guitierrez), Mélanie Armante, John Bally, Cara Battersby, Mélisse Bonfand, Leonardo Bronfman ‎, Nathalie Brouillet, Gemma Busquet, Desmond Jeff , Daniel Díaz, James Di Francesco, Gilberto C. Gomez, Matthias Gonzalez, Estrella Guzman, Patrick Hennebelle, Fabrice Herpin, Alexander Howard, Isabelle Joncour, Bilal Ladjelate, Yueh-ning Lee, Bertrand Le Floch, Pierre Lesaffre, Yuxin Lin, Ken Marsh, Anaelle Maury, Sasha Men’shchikov, Karl Menten, Estelle Moraux, Lee Mundy, Quang Nguyen Luong, Satoshi Ohashi, Marc Pound, Nicolas Reyes, Theo Richardson, Pedro Ruben Rivera Ortiz, Jean-Francois Robitaille, Erik Rosolowsky, Takeshi Sakai, Frédéric Schuller, Daniel Walker, Anthony Whitworth, Benjamin Wu, Friedrich Wyrowski

(How) does the core mass function (CMF) map to the stellar initial mass function (IMF)?


Konyves+ 2015

(How) does the core mass function (CMF) map to the stellar initial mass function (IMF)?


Konyves+ 2015

(How) does the core mass function (CMF) map to the stellar initial mass function (IMF)?


Offner+ 2014

ALMA-IMF Initial Results

  • Data Paper:
    • High dynamic range images
    • Careful treatment of continuum
    • Millimeter spectral index maps
  • Hundreds of cores measured in multiple cloud evolutionary stages
    • Uniform beam and sensitivity
    • First samples to include massive (M>10) cores
  • Evolution of the CMF with region age

ALMA-IMF Data Soon

  • Continuum data paper in prep (Ginsburg+, with big data reduction team: Roberto Galvan-Madrid, Nichol Cunningham, Timea Csengeri, Patricio Sanhueza, Fernando Olguin, Thomas Nony, Jordan Molet, Ana Lopez, Yohan Pouteau, Andrez Guzman, Manuel Fernandez, Melisse Bonfand)
    • Self-calibration (10-500% dynamic range improvement)
    • Mosaicing
    • Continuum selection
    • Method comparison
  • Survey overview paper in prep (Motte+)
    • Sample selection (evolutionary stages), highlights
  • Catalog paper in prep (Louvet+)
    • ~1000 cores cataloged

ALMA-IMF data highlights

Core measurements: Massive cores in massive clusters
Core measurements: 1000-2000 AU resolution

Measurements of the CMF

The CMF does not appear to be universal
Recent ALMA CMF measurements:
Heterogeneous source extraction, opacity & temperature assumption

ALMA-IMF Early Results:
The CMF steepens with time?

Louvet+, in prep

Self-Calibration (B3)

G010.62
G012.80
G327.29
G328.25
G333.60
G337.92
G338.93
G351.77
G353.41
W43-MM1
W43-MM2
W43-MM3
W51-E
W51-IRS2

Self-Calibration (B6)

G010.62
G012.80
G327.29
G328.25
G333.60
G337.92
G338.93
G351.77
G353.41
W43-MM1
W43-MM2
W43-MM3
W51-E
W51-IRS2

BSENS vs CLEANEST (B6)

G008
G010.62
G012.80
G327.29
G328.25
G333.60
G337.92
G338.93
G351.77
G353.41
W43-MM2
W43-MM2
W43-MM3
W51-E
W51-IRS2
BSENS - Cleanest: G333 B6
BSENS - Cleanest: W51-IRS2 B3

Spectral Index

We used α maps (& others) to assess ages of regions.

On the Rayleigh-Jeans tail:
  • Dust: α > 2 (β > 0 )
  • Free-free: α ~ 0.1
  • Synchrotron: α < 1
  • Optically Thick: α = 2
    (no mechanism implied!)
α map: G008

α map: G10

α map: G338

α map: W51IRS2

Fraction of area filled with free-free emission is a coarse tracer of evolutionary stage

ALMA-IMF Initial Results

  • Data Paper:
    • High dynamic range images
    • Careful treatment of continuum
    • Millimeter spectral index maps
  • Hundreds of cores measured in multiple cloud evolutionary stages
    • Uniform beam and sensitivity
    • First samples to include massive (M>10) cores
  • Evolution of the CMF with region age
Robust Comparisons: G008.67 B3
Robust Comparisons: G008.67 B6
Robust Comparisons: G010.62 B3
Robust Comparisons: G010.62 B6
Robust Comparisons: G012.80 B3
Robust Comparisons: G012.80 B6
Robust Comparisons: G327.29 B3
Robust Comparisons: G327.29 B6
Robust Comparisons: G328.25 B3
Robust Comparisons: G328.25 B6
Robust Comparisons: G333.60 B3
Robust Comparisons: G333.60 B6
Robust Comparisons: G337.92 B3
Robust Comparisons: G337.92 B6
Robust Comparisons: G338.93 B3
Robust Comparisons: G338.93 B6
Robust Comparisons: G351.77 B3
Robust Comparisons: G351.77 B6
Robust Comparisons: G353.41 B3
Robust Comparisons: G353.41 B6
Robust Comparisons: W43-MM1 B3
Robust Comparisons: W43-MM2 B3
Robust Comparisons: W43-MM2 B6
Robust Comparisons: W43-MM3 B3
Robust Comparisons: W43-MM3 B6
Robust Comparisons: W51-E B3
Robust Comparisons: W51-E B6
Robust Comparisons: W51-IRS2 B3
Robust Comparisons: W51-IRS2 B6

Flux histograms

: G008
Outset: Histogram of all data.
Inset: Zoom-in, with linear X-scale, near zero.
Inset, sub: histogram minus Gaussian model.
G10
G12
G327
G328
G333
G337
G338
G351
G353
W43MM2
W43MM3
W51-E
W51IRS2

UV Histograms: Effective resolution, LAS

G008 B3
G008.67 B6
G010.62 B3
G010.62 B6
G012.80 B3
G012.80 B6
G327.29 B3
G327.29 B6
G328.25 B3
G328.25 B6
G333.60 B3
G333.60 B6
G337.92 B3
G337.92 B6
G338.93 B3
G338.93 B6
G351.77 B3
G351.77 B6
G353.41 B3
G353.41 B6
W43-MM1 B3
W43-MM2 B3
W43-MM2 B6
W43-MM3 B3
W43-MM3 B6
W51-E_B3
W51-E_B6
W51-IRS2_B3
W51-IRS2_B6
Paper figures: table plots
Continuum Selection>

Continuum Selection

α map: G008
α map: G10
α map: G12
α map: G327
α map: G328
α map: G333
α map: G337
α map: G338
α map: G351
α map: G353
α map: W43MM2
α map: W43MM3
α map: W51Ee2
α map: W51Ee8
α map: W51EIRS1
α map: W51IRS2

Histogram of spectral index

G008
G10
G12
G327
G328
G333
G337
G338
G351
G353
W43MM2
W43MM3
W51-E
W51IRS2

BSENS self-calibrated (B3)

G010.62
G012.80
G327.29
G328.25
G333.60
G337.92
G338.93
G351.77
G353.41
W43-MM1
W43-MM2
W43-MM3
W51-E
W51-IRS2

BSENS vs CLEANEST (B3) - G008

G010.62
G012.80
G327.29
G328.25
G333.60
G337.92
G338.93
G351.77
G353.41
W43-MM1
W43-MM2
W43-MM3
W51-E
W51-IRS2