Low-mass star formation and the initial mass function in the ρ Ophiuchi cloud core

K. L. Luhman, George H. Rieke

Research output: Contribution to journalArticle

192 Citations (Scopus)

Abstract

We have obtained moderate-resolution (R = 800-1200) K-band spectra for ∼100 stars within and surrounding the cloud core of ρ Oph. We have measured spectral types and continuum veilings and have combined this information with results from new deep imaging. Using the latest evolutionary tracks of D'Antona & Mazzitelli to interpret the H-R diagram for ρ Oph, we infer ages ranging between 0.1 and 1 Myr for the class II and III sources (i.e., those that have emerged from their natal cocoons). A few stars may be slightly older. The initial mass function (IMF) peaks at about 0.4 M and slowly declines to the hydrogen-burning limit with a slope of ∼ -0.5 in logarithmic units (Salpeter is +1.35). Our lower limits on the numbers of substellar objects demonstrate that the IMF probably does not fall more steeply below the hydrogen-burning limit, at least down to ∼0.02 M. The derived IMF is consistent with previous findings that the ρ Oph IMF is roughly flat from 0.05 to 1 M. The exact shape of the mass function remains a function of the theoretical evolutionary tracks and, at the lowest masses, the conversion from spectral types to effective temperatures. We then make the first comparison of mass functions of stars and prestellar clumps measured in the same region. The similar behavior of the two mass functions in ρ Oph supports the suggestion of Motte et al. and Testi & Sargent that the stellar mass function in young clusters is a direct product of the process of cloud fragmentation. We have also studied the very young and often still embedded class I and flat-spectrum objects. After considering the effect of extinction on the SED classifications of the sample, we find that ∼17% of the ρ Oph stars are class I, implying ∼0.1 Myr for the lifetime of this stage. In spectra separated by 2 yr, we observe simultaneous variability in the Brγ emission and K-band continuum veiling for two stars, where the hydrogen emission is brighter in the more heavily veiled data. This behavior indicates that the disk may contribute significantly to continuous K-band emission, in contrast to the proposal that the infalling envelope always dominates. Our detection of strong 2 μm veiling (rK = 1-4) in several class II and III stars, which should have disks but little envelope material, further supports this proposition. We also detect absorption features in the spectra of ∼25% of class I and flat-spectrum sources, demonstrating the feasibility of studying the photospheres of extremely young protostars.

Original languageEnglish (US)
Pages (from-to)440-465
Number of pages26
JournalAstrophysical Journal
Volume525
Issue number1 PART 1
StatePublished - Nov 1 1999

Fingerprint

Ophiuchi clouds
star formation
stars
extremely high frequencies
hydrogen
envelopes
continuums
cocoon
protostars
clumps
photosphere
stellar mass
suggestion
proposals
fragmentation
extinction

Keywords

  • Infrared: stars
  • Open clusters and associations: individual (ρ Ophiuchi)
  • stars: evolution
  • stars: low-mass, brown dwarfs
  • Stars: luminosity function, mass function
  • Stars: pre-main-sequence

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Low-mass star formation and the initial mass function in the ρ Ophiuchi cloud core. / Luhman, K. L.; Rieke, George H.

In: Astrophysical Journal, Vol. 525, No. 1 PART 1, 01.11.1999, p. 440-465.

Research output: Contribution to journalArticle

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N2 - We have obtained moderate-resolution (R = 800-1200) K-band spectra for ∼100 stars within and surrounding the cloud core of ρ Oph. We have measured spectral types and continuum veilings and have combined this information with results from new deep imaging. Using the latest evolutionary tracks of D'Antona & Mazzitelli to interpret the H-R diagram for ρ Oph, we infer ages ranging between 0.1 and 1 Myr for the class II and III sources (i.e., those that have emerged from their natal cocoons). A few stars may be slightly older. The initial mass function (IMF) peaks at about 0.4 M⊙ and slowly declines to the hydrogen-burning limit with a slope of ∼ -0.5 in logarithmic units (Salpeter is +1.35). Our lower limits on the numbers of substellar objects demonstrate that the IMF probably does not fall more steeply below the hydrogen-burning limit, at least down to ∼0.02 M⊙. The derived IMF is consistent with previous findings that the ρ Oph IMF is roughly flat from 0.05 to 1 M⊙. The exact shape of the mass function remains a function of the theoretical evolutionary tracks and, at the lowest masses, the conversion from spectral types to effective temperatures. We then make the first comparison of mass functions of stars and prestellar clumps measured in the same region. The similar behavior of the two mass functions in ρ Oph supports the suggestion of Motte et al. and Testi & Sargent that the stellar mass function in young clusters is a direct product of the process of cloud fragmentation. We have also studied the very young and often still embedded class I and flat-spectrum objects. After considering the effect of extinction on the SED classifications of the sample, we find that ∼17% of the ρ Oph stars are class I, implying ∼0.1 Myr for the lifetime of this stage. In spectra separated by 2 yr, we observe simultaneous variability in the Brγ emission and K-band continuum veiling for two stars, where the hydrogen emission is brighter in the more heavily veiled data. This behavior indicates that the disk may contribute significantly to continuous K-band emission, in contrast to the proposal that the infalling envelope always dominates. Our detection of strong 2 μm veiling (rK = 1-4) in several class II and III stars, which should have disks but little envelope material, further supports this proposition. We also detect absorption features in the spectra of ∼25% of class I and flat-spectrum sources, demonstrating the feasibility of studying the photospheres of extremely young protostars.

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KW - Stars: luminosity function, mass function

KW - Stars: pre-main-sequence

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