CO Observations of a FeLoBAL Quasar with an H alpha Absorption Line at z=2.3

SDSS J083942.11+380526.3 is an Iron Low-ionization Broad Absorption Line (FeLoBAL) quasar at z = 2.3, and Aoki et al. (2006) recently found the presence of an H alpha absorption line in the broad H alpha emission line. Motivated by an idea that this quasar may be a huge molecular gas reservoir in the early phase of quasar evolution, we made CO(J=3-2) observations of it using the Nobeyama Millimeter Array. No significant CO emission was detected; although an emission-like feature (2.5 sigma) was seen close (~ 2") to the quasar, we regard it as a noise. The obtained 3 sigma upper limit on the CO luminosity is L'_{{\rm CO}(J=3-2)} = 4.5 \times 10^{10} K km/s pc^2, which corresponds to M({\rm H}_2) = 3.6 times 10^10 M_{\odot} if we adopt the CO-to-H_2 conversion factor of 0.8 M_{\odot} (K km/s pc^2)^{-1}. This upper limit is comparable to L'_{{\rm CO}(J=3-2)} (and thus the molecular gas mass) detected in quasars and BAL quasars at z=1-3, and no sign of the presence of the huge amount of molecular gas in this FeLoBAL quasar was obtained.Comment: 7 pages, 1 figure. Accepted by PAS

Observing Supernova Neutrino Light Curves with Super-Kamiokande. III. Extraction of Mass and Radius of Neutron Stars from Synthetic Data

Neutrinos are guaranteed to be observable from the next Galactic supernova (SN). Optical light and gravitational waves are also observable, but may be difficult to observe if the location of the SN in the Galaxy or the details of the explosion are unsuitable. The key to observing the next SN is to first use neutrinos to understand various physical quantities and then link them to other signals. In this paper, we present Monte Carlo sampling calculations of neutrino events from Galactic SN explosions observed with Super-Kamiokande. The analytical solution of neutrino emission, which represents the long-term evolution of the neutrino light curve from SNe, is used as a theoretical template. It gives the event rate and event spectrum through inverse beta decay interactions with explicit model parameter dependence. Parameter estimation is performed on these simulated sample data by fitting least squares using the analytical solution. The results show that the mass, radius, and total energy of a remnant neutron star produced by an SN can be determined with an accuracy of ∼ 0.1 M⊙, ∼1 km, and ∼ 10⁵¹ erg, respectively, for a Galactic SN at 8 kpc

Leptomeningeal carcinomatosis in SCCP

Introduction: Leptomeningeal carcinomatosis in small cell carcinoma of the prostate is rare. Case presentation: A 69-year-old man visited our hospital due to dysuria and edema. Bilateral hydronephrosis and lymph node metastases due to a pelvic tumor were observed. Although the prostate-specific antigen level was normal, the tumor was suspected to originate from the prostate. He underwent percutaneous nephrostomy and prostate biopsy. Histopathology revealed small cell carcinoma accompanied by increased pro-gastrin-releasing peptide and neuron-specific enolase levels. After receiving systemic chemotherapy with carboplatin and etoposide and radiation therapy for prostate, these lesions gradually decreased in size, and tumor markers normalized. Ten months after the initial diagnosis, he developed consciousness disorder and seizure. Magnetic resonance imaging revealed leptomeningeal carcinomatosis without any other recurrences and elevated tumor markers. He died 4 weeks after these symptoms appeared. Conclusion: Careful monitoring of the central nervous system should be considered in small cell carcinoma of the prostate patients