A census of the young cluster IC 348

K. L. Luhman, John R. Stauffer, A. A. Muench, George H. Rieke, E. A. Lada, J. Bouvier, C. J. Lada

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Abstract

We present a new census of the stellar and substellar members of the young cluster IC 348. We have obtained images at I and Z for a 42′ × 28′ field encompassing the cluster and have combined these measurements with previous optical and near-infrared photometry. From spectroscopy of candidate cluster members appearing in these data, we have identified 122 new members, 15 of which have spectral types of M6.5-M9, corresponding to masses of ∼0.08-0.015 M by recent evolutionary models. The latest census for IC 348 now contains a total of 288 members, 23 of which are later than M6 and thus are likely to be brown dwarfs. From an extinction-limited sample of members (AV ≤ 4) for a 16′ × 14′ field centered on the cluster, we construct an initial mass function (IMF) that is unbiased in mass and nearly complete for M/M ≥ 0.03 (≲M8). In logarithmic units where the Salpeter slope is 1.35, the mass function for IC 348 rises from high masses down to a solar mass, rises more slowly down to a maximum at 0.1-0.2 M, and then declines into the substellar regime. In comparison, the similarly derived IMF for Taurus from Briceño et al. and Luhman et al. rises quickly to a peak near 0.8 M and steadily declines to lower masses. The distinctive shapes of the IMFs in IC 348 and Taurus are reflected in the distributions of spectral types, which peak at M5 and K7, respectively. These data provide compelling, model-independent evidence for a significant variation of the IMF with star-forming conditions.

Original languageEnglish (US)
Pages (from-to)1093-1115
Number of pages23
JournalAstrophysical Journal
Volume593
Issue number2 I
DOIs
StatePublished - Aug 20 2003

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census
young
infrared photometry
IMF
near infrared
extinction
spectroscopy
slopes
stars

Keywords

  • Infrared: stars
  • Stars: evolution
  • Stars: formation
  • Stars: low-mass, brown dwarfs
  • Stars: luminosity function, mass function
  • Stars: pre-main-sequence

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Luhman, K. L., Stauffer, J. R., Muench, A. A., Rieke, G. H., Lada, E. A., Bouvier, J., & Lada, C. J. (2003). A census of the young cluster IC 348. Astrophysical Journal, 593(2 I), 1093-1115. https://doi.org/10.1086/376594

A census of the young cluster IC 348. / Luhman, K. L.; Stauffer, John R.; Muench, A. A.; Rieke, George H.; Lada, E. A.; Bouvier, J.; Lada, C. J.

In: Astrophysical Journal, Vol. 593, No. 2 I, 20.08.2003, p. 1093-1115.

Research output: Contribution to journalArticle

Luhman, KL, Stauffer, JR, Muench, AA, Rieke, GH, Lada, EA, Bouvier, J & Lada, CJ 2003, 'A census of the young cluster IC 348', Astrophysical Journal, vol. 593, no. 2 I, pp. 1093-1115. https://doi.org/10.1086/376594
Luhman KL, Stauffer JR, Muench AA, Rieke GH, Lada EA, Bouvier J et al. A census of the young cluster IC 348. Astrophysical Journal. 2003 Aug 20;593(2 I):1093-1115. https://doi.org/10.1086/376594
Luhman, K. L. ; Stauffer, John R. ; Muench, A. A. ; Rieke, George H. ; Lada, E. A. ; Bouvier, J. ; Lada, C. J. / A census of the young cluster IC 348. In: Astrophysical Journal. 2003 ; Vol. 593, No. 2 I. pp. 1093-1115.
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AU - Stauffer, John R.

AU - Muench, A. A.

AU - Rieke, George H.

AU - Lada, E. A.

AU - Bouvier, J.

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N2 - We present a new census of the stellar and substellar members of the young cluster IC 348. We have obtained images at I and Z for a 42′ × 28′ field encompassing the cluster and have combined these measurements with previous optical and near-infrared photometry. From spectroscopy of candidate cluster members appearing in these data, we have identified 122 new members, 15 of which have spectral types of M6.5-M9, corresponding to masses of ∼0.08-0.015 M⊙ by recent evolutionary models. The latest census for IC 348 now contains a total of 288 members, 23 of which are later than M6 and thus are likely to be brown dwarfs. From an extinction-limited sample of members (AV ≤ 4) for a 16′ × 14′ field centered on the cluster, we construct an initial mass function (IMF) that is unbiased in mass and nearly complete for M/M⊙ ≥ 0.03 (≲M8). In logarithmic units where the Salpeter slope is 1.35, the mass function for IC 348 rises from high masses down to a solar mass, rises more slowly down to a maximum at 0.1-0.2 M⊙, and then declines into the substellar regime. In comparison, the similarly derived IMF for Taurus from Briceño et al. and Luhman et al. rises quickly to a peak near 0.8 M ⊙ and steadily declines to lower masses. The distinctive shapes of the IMFs in IC 348 and Taurus are reflected in the distributions of spectral types, which peak at M5 and K7, respectively. These data provide compelling, model-independent evidence for a significant variation of the IMF with star-forming conditions.

AB - We present a new census of the stellar and substellar members of the young cluster IC 348. We have obtained images at I and Z for a 42′ × 28′ field encompassing the cluster and have combined these measurements with previous optical and near-infrared photometry. From spectroscopy of candidate cluster members appearing in these data, we have identified 122 new members, 15 of which have spectral types of M6.5-M9, corresponding to masses of ∼0.08-0.015 M⊙ by recent evolutionary models. The latest census for IC 348 now contains a total of 288 members, 23 of which are later than M6 and thus are likely to be brown dwarfs. From an extinction-limited sample of members (AV ≤ 4) for a 16′ × 14′ field centered on the cluster, we construct an initial mass function (IMF) that is unbiased in mass and nearly complete for M/M⊙ ≥ 0.03 (≲M8). In logarithmic units where the Salpeter slope is 1.35, the mass function for IC 348 rises from high masses down to a solar mass, rises more slowly down to a maximum at 0.1-0.2 M⊙, and then declines into the substellar regime. In comparison, the similarly derived IMF for Taurus from Briceño et al. and Luhman et al. rises quickly to a peak near 0.8 M ⊙ and steadily declines to lower masses. The distinctive shapes of the IMFs in IC 348 and Taurus are reflected in the distributions of spectral types, which peak at M5 and K7, respectively. These data provide compelling, model-independent evidence for a significant variation of the IMF with star-forming conditions.

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KW - Stars: formation

KW - Stars: low-mass, brown dwarfs

KW - Stars: luminosity function, mass function

KW - Stars: pre-main-sequence

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