Michael R. Meyer, M. Andersen, D. Apai, J. Greissl, P. Hinz, M. Kenworthy, C.
Kulesa, D. McCarthy, W. Schlingman, Steward Observatory, University of Arizona
with Bruce Wilking, UM-St. Louis, and Lori Allen, CfA
Searching for Our Origins: Star and Planet Formation with the MMT
To understand chemical evolution. Interpret the integrated light of other
galaxies. Constrain contribution to baryonic
dark matterThe shape of the initial mass function provides
crucial information concerning the origins of
stellar masses.
● Are there characteristic masses?● Is the IMF truly universal?
Why Study the IMF?
Red Channel Spectrum of Young Brown Dwarf in rho Oph with OLD MMT
Wilking, Greene, and Meyer, 1999, AJ, 117, 469.
FLAMINGOS Imaging of Rho Oph with the new MMT
Wilking, Meyer, and Allen (2006).
Near-IR Color-Magnitude Diagram and PMS H-R Diagram
FLAMINGOS on the MMT (Wilking, Meyer, and Allen)
FLAMINGOS on the MMT (Wilking, Meyer, and Allen)
Color_1
Col
or_2
Star+Dust Star+
Dust+Disk
Star
Star+Disk
FSPEC on the NEW MMT Effects of Surface Gravity on Near-IR Spectra
Gorlova, Meyer, Rieke, & Liebert, 2003, ApJ, 93, 1047.
Is the IMF different insuper-star clusters?
ARIESArizona Infrared Imager and Echelle Spectrograph
Aries “purple”: 1-2.5 um imager, in operation since 2003
and...
Aries “green”: long slit and echelle spectrometer, designed for 1-5 um, arriving winter 2006-7
Aries Contacts:Don McCarthy (PI)
Craig Kulesa
ARIES Imaging
1-2.5 um (1k x 1k HgCdTe)
- f/15 imager: 0.038”/pix (40” FOV)- f/30 imager: 0.019”/pix (20” FOV)- slit viewer for Aries “green”
new Si grism: slitless spectroscopy w/ 2 pixel R=5000
ARIES Spectroscopy
2006: 1-2.5 um (1k x 1k HgCdTe)2007: 1-5 um (2k x 2k HgCdTe)
Long slit mode: 90” long0.2-0.4” wideR ~ 2000-5000
Echelle mode: 1” long0.1” to 0.4” wideR ~ 15,000 to 60,000cross-dispersed
Imaging mode: 0.1”/pix
Aries “purple” and Aries “green” operate simultaneously!
Extreme Star Formation: W51- High Luminosity UCHII Region. - 130 stars > 10 Msun.- 7 kpc.- Av = 5-10 mag.- < 3 Myr old.(Okumura et al. 2000)
- MMT-AO.- ARIES Camera.- 0.14” @ K-band.- 40” FOV. - 10 sigma K < 21m.- Reach HBL Av < 30 m in 1 hr.
Meyer et al. (2004); Andersen et al. (2005).
<= Near-IR CMDFor Av-limited
sample calculateratio of high-to-low
mass stars in W51
Expectation =>Probably of observingratio for various IMFs
MMT-AO Engineering PSF Simulated Trapezium Observations R(Sky Noise) = 1 Rc = 0.2 pc from Close et al. 2003. using Hillenbrand & Carpenter (2000). Hcomp(at Rc) < 24 mag
R(sky noise) = 2.5 Rc = 0.5 pc R(Sky Noise) = 4 Rc = 0.8 pc R(Sky Noise) > 20 Rc = 4-5 pc Hcomp(at Rc) < 17.8 mag. Hcomp(at Rc) < 15.3 mags. Core Radius not resolved.
25 kpc 50 kpc 0.5 Mpc
5 kpcPSF 0.5 kpc
The Trapezium on the Bleeding Edge: Sensitivity vs. Confusion...
2D Classificationfrom R=100 NIR Narrow-Bands(Meyer et al. 1998;Wallace et al. 2000)
Unresolved Super Star Clusters
in NGC 4038/4039
Mengel et al. (2002)
***
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Ca Mg CO(2-0)
3 Myr
1 Myr
3 Myr
1 Myr
Age
6.44 +/- 0.30Ch03
6.27 +/- 0.44Ch03
11.01 +/- 0.44S55
8.98 +/- 0.82S55
EW(CaI +
CO(2-0))/EW(MgI)
IMF
S55 1 Myr
S55 3 Myr
Ch03 1 Myr
Ch03 3Myr
Meyer & Greissl, 2005, ApJL
IMF in Antennae Very Young SSC #6?
Greissl, Meyer, Christopher, & Scoville (2006)
“UD” HII Regions
(Proto-SSCs)
Johnson et al. (2001)
12”
Warm Debris Surrounding Sun-like Stars
Michael R. Meyer
Steward Observatory, The University of
Arizona D. Backman (NASA-Ames, D.P.I.) , S.V.W. Beckwith (STScI), J. Bouwman
(MPIA), T. Brooke (Caltech), J.M. Carpenter (Caltech), M. Cohen (UC-
Berkeley), U. Gorti (NASA-Ames), T. Henning (MPIA), L. Hillenbrand (Caltech,
D.P.I.), D. Hines (SSI), D. Hollenbach (NASA-Ames), J. Lunine (LPL), J.S. Kim
(Steward), R. Malhotra (LPL), E. Mamajek (CfA), A. Moro-Martin (Princeton ),
P. Morris (SSC), J. Najita (NOAO), D. Padgett (SSC), I. Pascucci (Steward), J.
Rodmann (MPIA), W. Schlingman (Steward), M. Silverstone (Steward), D.
Soderblom (STScI), J.R. Stauffer (SSC), B. Stobie (Steward), S. Strom
(NOAO), D. Watson (Rochester), S. Weidenschilling (PSI), S. Wolf (MPIA),
and E. Young (Steward).
Spitzer IRS/MIPS Reveals ``Needle'' in FEPS Haystack
Hines et al. (2006, ApJ, 638, 1070)
HD 12039 IR Excess: Temperature ~ 110 K – warm!
Hines et al. (2006, ApJ, 638, 1070)
Warm Debris and the Formation of Habitable Planets
(Cf. Meyer et al. 2006; Kenyon and Bromley, 2005)
Spectroscopic Observations of Transient
Dust Debris Surrounding Sun-like Stars
Beichman et al. (ApJ, 2005); See also Hines et al. (ApJ, 2006)
MIR