We have completed a 1.1 mm continuum survey of 7.5 deg 2 of the Perseus Molecular Cloud using Bolocam at the Caltech Submillimeter Observatory. This represents the largest millimeter or submillimeter continuum map of Perseus to date. Our map covers more than 30,000 31 ′′ (FWHM) resolution elements to a 1σ RMS of 15 mJy/beam. We detect a total of 122 cores above a 5σ point source mass detection limit of 0.18M ⊙ , assuming a dust temperature of T D = 10 K, 60 of which are new millimeter or submillimeter detections. The 1.1 mm mass function is consistent with a broken power law of slope α 1 = 1.3 (0.5M ⊙ < M < 2.5M ⊙ ) and α 2 = 2.6 (M > 2.5M ⊙ ), similar to the local initial mass function slopeNo more than 5% of the total cloud mass is contained in discrete 1.1 mm cores, which account for a total mass of 285M ⊙ . We suggest an extinction threshold for millimeter cores of A V ∼ 5 mag, based on our calculation of the probability of finding a 1.1 mm core as a function Recent estimates of the distance to Perseus range from 220 pc to 350 pc (e. g Černis 1990;Herbig & Jones 1983). Larger values (300 − 350 pc) are often adopted based on the

We present results of a new deep 1.1 mm survey using Bolocam, a millimeter-wavelength bolometer array camera designed for mapping large fields at fast scan rates, without chopping. A map, galaxy candidate list, and derived number counts are presented. This survey encompasses 324 arcmin 2 to an rms noise level (filtered for point sources) of 1:1 mm ' 1:4 mJy beam À1 and includes the entire regions surveyed by the published 8 mJy 850 m JCMT SCUBA and 1.2 mm IRAM MAMBO surveys. We reduced the data using a custom software pipeline to remove correlated sky and instrument noise via a principal component analysis. Extensive simulations and jackknife tests were performed to confirm the robustness of our source candidates and estimate the effects of false detections, bias, and completeness. In total, 17 source candidates were detected at a significance !3.0 , with six expected false detections. Nine candidates are new detections, while eight candidates have coincident SCUBA 850 m and /or MAMBO 1.2 mm detections. From our observed number counts, we estimate the underlying differential number count distribution of submillimeter galaxies and find it to be in general agreement with previous surveys. Modeling the spectral energy distributions of these submillimeter galaxies after observations of dusty nearby galaxies suggests extreme luminosities of L ¼ ð1:0 1:6Þ ; 10 13 L and, if powered by star formation, star formation rates of 500-800 M yr À1 .

Taking advantage of an improved genetic optimization algorithm for fitting unconstrained Kepler orbits to the Hipparcos intermediate astrometric data, we obtain additional orbital solutions for 81 Hipparcos stars with previous stochastic (failed) solutions. The sample includes astrophysically interesting objects, including the old disk wide binary HIP 754, the nearby AGB star HIP 34922 (L 2 Pup), and the nearby M2 dwarf HIP 5496 (GJ 54, at 8 pc from the Sun), which has a resolved M dwarf companion.

We perform a fluctuation analysis of the 1.1 mm Bolocam Lockman Hole Survey, which covers 324 arcmin 2 to a very uniform point-source-filtered rms noise level of ' 1:4 mJy beam À1 . The fluctuation analysis has the significant advantage of using all of the available data, since no extraction of sources is performed: direct comparison is made between the observed pixel flux density distribution [P(D)] and the theoretical distributions for a broad range of power-law number count models, n(S ) ¼ n 0 S À . We constrain the number counts in the 1-10 mJy range and derive significantly tighter constraints than in previous work: the power-law index ¼ 2:7 þ0:18 À0:15 , while the amplitude is n 0 ¼ 1595. At flux densities above 4 mJy, where a valid comparison can be made, our results agree extremely well with those derived from the extracted source number counts by Laurent et al.: the best-fitting differential slope is somewhat shallower ( ¼ 2:7 vs. 3.2), but well within the 68% confidence limit, and the amplitudes (number of sources per square degree) agree to 10%. At 1 mJy, however [the limit of the P(D) analysis], the shallower slope derived here implies a substantially smaller amplitude for the integral number counts than extrapolation from above 4 mJy would predict. Our derived normalization is about 2.5 times smaller than that determined by the Max-Planck Millimeter Bolometer (MAMBO) at 1.2 mm (Greve et al.). However, the uncertainty in the normalization for both data sets is dominated by the systematic (i.e., absolute flux calibration) rather than statistical errors; within these uncertainties, our results are in agreement. Our best-fit amplitude at 1 mJy is also about a factor of 3 below the prediction of Blain et al., but we are in agreement above a few millijanskys. We estimate that about 7% of the 1.1 mm background has been resolved at 1 mJy.

ABSTRACT16.5, and 22.5 cm Ϫ1 , respectively. Using models for the brightness temperature of Mars, we also give the whole-disk brightness temperatures for Jupiter and Saturn for the four frequencies.