Final Targeting Strategy for the SDSS-IV APOGEE-2S Survey

APOGEE is a high-resolution (R ∼ 22,000), near-infrared, multi-epoch, spectroscopic survey of the Milky Way. The second generation of the APOGEE project, APOGEE-2, includes an expansion of the survey to the Southern Hemisphere called APOGEE-2S. This expansion enabled APOGEE to perform a fully panoramic mapping of all of the main regions of the Milky Way; in particular, by operating in the H band, APOGEE is uniquely able to probe the dust-hidden inner regions of the Milky Way that are best accessed from the Southern Hemisphere. In this paper we present the targeting strategy of APOGEE-2S, with special attention to documenting modifications to the original, previously published plan. The motivation for these changes is explained as well as an assessment of their effectiveness in achieving their intended scientific objective. In anticipation of this being the last paper detailing APOGEE targeting, we present an accounting of all such information complete through the end of the APOGEE-2S project; this includes several main survey programs dedicated to exploration of major stellar populations and regions of the Milky Way, as well as a full list of programs contributing to the APOGEE database through allocations of observing time by the Chilean National Time Allocation Committee and the Carnegie Institution for Science. This work was presented along with a companion article, Beaton et al. (2021), presenting the final target selection strategy adopted for APOGEE-2 in the Northern Hemisphere.

Behind the curve: a comparison of historical sources for the Carnegie curve of the global atmospheric electric circuit

The “Carnegie curve” describes the diurnal variation of the global atmospheric electric circuit. It was originally found from atmospheric electric potential gradient (PG) measurements made on the Carnegie, effectively a floating atmospheric electrical observatory, which undertook global cruises between 1915 and 1929. These measurements confirmed that the single diurnal cycle PG variation, previously obtained in both polar regions, was global in extent. The averaged diurnal PG variation, represented by derived harmonic fits, provides a characteristic variation known as the “Carnegie curve”, against which modern measurements are still compared. The ocean air PG measurements were extensively described in reports of the Carnegie Institution of Washington (CIW) but widely used secondary sources of the Carnegie curve contain small differences, arising through approximations and transcription errors. Investigations using the historical CIW data show that the original harmonic fit coefficients are reproducible. Despite the inconsistencies, the secondary sources nevertheless mostly yield diurnal variations which fall within the variability of the original historical data.

Digitization of the Carnegie Analog Broadband Instruments Tape Records (1965–1996)

Between 1965 and 2003, the Carnegie Institution of Washington’s Department of Terrestrial Magnetism operated a continuous network of nine broadband seismographs with locations in South America, Japan, Iceland, Papua New Guinea, and Washington, D.C. The Carnegie seismographs designed in the 1960s by Selwyn Sacks were among the earliest broadband instruments, sensing between at least 30 s and ∼30 Hz. Given the scarcity of historic seismic data of comparable bandwidth and dynamic range prior to the widespread shift to force-feedback instruments and digital recording around the mid-1980s, this dataset is still of high scientific value today. The Carnegie seismographs recorded data to magnetic tapes meant to be read and analyzed using a custom playback system. Since 1989 these tapes have been stored in a climate-controlled, electromagnetically shielded room, which preserved them in reasonably good condition. However, some tapes now show signs of moisture damage, and reading them is difficult and time consuming by today’s standards, creating a barrier to the use of this dataset. To overcome these issues, we have undertaken an ongoing effort to digitize this dataset with the goal of making it publicly available in Standard for the Exchange of Earthquake Data (SEED) format at the Incorporated Research Institutions for Seismology Data Management Center (IRIS DMC).

Temperatura efectiva en estrellas de tipo solar

Temperatura efectiva en estrellas de tipo solar D. Cornejo, I. Ramírez, P. Barklem, W. Guevara Dirección de Astrofísica, Comisión Nacional de Investigación y Desarrollo Aeroespacial - CONIDA, Luis Felipe Villarán 1069, San Isidro, Lima, Perú. The Observatories of the Carnegie Institution for Science; 813 Santa Barbara Street, Pasadena, CA 91101, USA. Department of Astronomy and Space Physics, Uppsala University, Box 515, 751-20 Uppsala, Sweden DOI: https://doi.org/10.33017/RevECIPeru2011.0027/ RESUMEN Este trabajo consiste en determinar la temperatura efectiva de una muestra de 62 estrellas de tipo solar mediante el método de ajuste de perfiles teóricos a la linea espectral Hα (6562.8 A). Las estrellas analizadas han sido observadas usando el Telescopio Harlan J. Smith de 2.7 m del Observatorio McDonald de la Universidad de Texas mientras que los perfiles teóricos se basan en modelos de atmósferas estelares y teoría cuántica mas recientes. Nuestros resultados poseen un margen de error interno de ≈ 20 K, lo cual nos permite comparar nuestras temperaturas con aquellas determinadas usando otros métodos y especular sobre el origen de las diferencias observadas. Descriptores: Perfiles de lineas espectrales, atmósferas estelares. ABSTRACT The effective temperature for a sample of 62 solar-type stars has been determined fitting theoretical spectral profiles to observed Hα lines (6562.8 A). The stars analyzed has been observed using the 2.7 m Harlan J. Smith telescope at the McDonald Observatory of the University of Texas. The theoretical profiles are based on recent models of stellar atmospheres and quantum theory. The calculated temperatures have internal errors of ≈ 20 K with other techniques and speculate about the origin of the observed differences. Keywords: Spectral line profiles, Stellar Atmospheres.

Expeditions for the observation in Sobral, Brazil, of the May 29, 1919 total solar eclipse

I report on the three expeditions organized to observe, in the Brazilian State of Ceará, the total solar eclipse on May 29, 1919. Apart from the well-known British expedition, which aimed to perform measurements of the bending of stellar light rays passing near the Sun, resulting in the confirmation of Einstein’s Theory of General Relativity, there were two other expeditions in that occasion. One has been a Brazilian expedition, organized by the National Observatory, with the aim of studying the solar corona. The other has been a North-American expedition, organized by the Carnegie Institution, aiming to perform measurements related to terrestrial magnetism and atmospheric electricity.

Mexican Indigenismo and the International Fraternity of Science

Mexican racial science developed in close relation to foreign scholars and institutions including Corrado Gini of Italy, a proponent of Latin eugenics, Franz Boas, the Carnegie Institution in Washington, the international eugenics movement, and the Pan-American child welfare movement. Along with the mobilization of rural peoples during the Mexican Revolution, growing international interest in Mexico and the international eugenics movement galvanized Mexican indigenismo, the state-sponsored movement championing the nation’s indigenous heritage. This chapter focuses on Manuel Gamio, who founded Mexico’s Dirección de Antropología and worked in the powerful Secretaría de Educación Pública (SEP). Gamio conveyed Mexican social science abroad and foreign social science to Mexico. He attempted to create a social science that was both “Mexican” and modern, but found it hard to delineate a modernity that could accommodate Mexico’s demographic heterogeneity. Gamio creatively reconciled Mexico’s demographic characteristics with liberal universalism and scientific rationality, yet still suffered the intellectual imperialism and condescension of his U.S. counterparts.

DIVISION F COMMISSION 53: EXTRASOLAR PLANETS

The IAU Working Group on Extrasolar Planets (WGESP) was created by the Executive Council as a Working Group of Division III. This decision took place in June 1999, that is only 7 years after the discovery of planets around the pulsar PSR B1257+12 and 4 years after the discovery of 51 Peg b. This working group was renewed for 3 years at the General Assembly in 2003 in Sydney, Australia. It was chaired by Alan Boss from Carnegie Institution of Washington. The WGESP members were Paul Butler, William Hubbard, Philip Ianna, Martin Kürster, Jack Lissauer, Michel Mayor, Karen Meech, Francois Mignard, Alan Penny, Andreas Quirrenbach, Jill Tarter, and Alfred Vidal-Madjar.