Search for very high energy Gamma radiation from the Starburst Galaxy IC 342

This thesis describes a search for very high energy (VHE) gamma-ray emission from the starburst galaxy IC 342. The analysis was based on data from the 2003 — 2004 observing season recorded using the Whipple 10-metre imaging atmospheric Cherenkov telescope located on Mount Hopkins in southern Arizona. IC 342 may be classed as a non-blazar type galaxy and to date only a few such galaxies (M 87, Cen A, M 82 and NGC 253) have been detected as VHE gamma-ray sources. Analysis of approximately 24 hours of good quality IC 342 data, consisting entirely of ON/OFF observations, was carried out using a number of methods (standard Supercuts, optimised Supercuts, scaled optimised Supercuts and the multivariate kernel analysis technique). No evidence for TeV gamma-ray emission from IC 342 was found. The significance was 0.6 a with a nominal rate of 0.04 ± 0.06 gamma rays per minute. The flux upper limit above 600 GeV (at 99.9 % confidence) was determined to be 5.5 x 10-8 m-2 s-1, corresponding to 8 % of the Crab Nebula flux in the same energy range.

Search for dark matter using VHE gamma-ray telescopes

One of the unresolved questions of modern physics is the nature of Dark Matter. Strong experimental evidences suggest that the presence of this elusive component in the energy budget of the Universe is quite significant, without, however, being able to provide conclusive information about its nature. The most plausible scenario is that of weakly interacting massive particles (WIMPs), that includes a large class of non-baryonic Dark Matter candidates with a mass typically between few tens of GeV and few TeVs, and a cross section of the order of weak interactions. Search for Dark Matter particles using very high energy gamma-ray Cherenkov telescopes is based on the model that WIMPs can self-annihilate, leading to production of detectable species, like photons. These photons are very energetic, and since unreflected by the Universe's magnetic fields, they can be traced straight to the source of their creation. The downside of the approach is a great amount of background radiation, coming from the conventional astrophysical objects, that usually hides clear signals of the Dark Matter particle interactions. That is why good choice of the observational candidates is the crucial factor in search for Dark Matter. With MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov Telescopes), a two-telescope ground-based system located in La Palma, Canary Islands, we choose objects like dwarf spheroidal satellite galaxies of the Milky Way and galaxy clusters for our search. Our idea is to increase chances for WIMPs detection by pointing to objects that are relatively close, with great amount of Dark Matter and with as-little-as-possible pollution from the stars. At the moment, several observation projects are ongoing and analyses are being performed.

Impacto de la circulación ecuatorial en la zona mínima de oxógeno presente en el norte del Ecosistema de la Corriente del Humboldt

El Norte del Ecosistema de la Corriente Humboldt (NECH) constituye una de las mayores zonas de afloramiento, localizada en el borde oriental del Pacifico Sur, la cual presenta características particulares, entre las que destacan una alta producción primaria y la presencia de una de las zonas mínimas de oxigeno (ZMO) más intensas en el océano abierto. La ZMO presente en esta zona es producto de la alta demanda de oxígeno durante la remineralización de la materia orgánica, el largo tiempo de residencia de sus aguas y su poca ventilación. En el presente estudio nos enfocamos en estudiar la influencia de cambios en la ventilación en la ZMO del NECH, tomando como las principales fuentes de aporte de oxígeno en esta zona a la Corriente Sub-superficial Ecuatorial (EUC) y las Contracorrientes Sub-superficiales del Sur (SSCCs) o también conocidas como los Jets de Tsuchiya. Utilizamos el modelo acoplado físico-biogeoquímico ROMS-PISCES, para observar la sensibilidad de la ZMO a diferentes condiciones de la circulación ecuatorial provenientes de dos modelos oceánicos de circulación general (SODA y MERCATOR). Los resultados muestran que el flujo de oxígeno a los 88ºW disminuye latitudinalmente de la EUC a los SSCCs; además, se observa que la ZMO desaparece de los 4ºN - 4ºS en la simulación que presenta una circulación más intensa (RPSoda) por lo que se puede concluir que una intensificación de la circulación ecuatorial afectaría principalmente a la zona ecuatorial y no frente a Perú, debido a que una mayor ventilación sería compensada con un mayor consumo de oxigeno durante la remineralización, producto de una alta productividad generada por un mayor flujo de nutrientes.

A search for microquasar candidates at low galactic latitudes

Recent studies of relativistic jet sources in the Galaxy, also known as microquasars, have been very useful in trying to understand the accretion/ejection processes that take place near compact objects. However, the number of sources involved in such studies is still small. In an attempt to increase the number of known microquasars we have carried out a search for new Radio Emitting X-ray Binaries (REXBs). These sources are the ones to be observed later with VLBI techniques to unveil their possible microquasar nature. To this end, we have performed a cross-identification between the X-ray ROSAT all sky survey Bright Source Catalog (RBSC) and the radio NRAO VLA Sky Survey (NVSS) catalogs under very restrictive selection criteria for sources with |b|<5 degrees. We have also conducted a deep observational radio and optical study for six of the selected candidates. At the end of this process two of the candidates appear to be promising, and deserve additional observations aimed to confirm their proposed microquasar nature.

One-sided jet at milliarcsecond scales in LSI+61·303

We present Very Long Baseline Interferometry (VLBI) observations of the high mass X-ray binary LSI+61303, carried out with the European VLBI Network (EVN). Over the 11 hour observing run, performed 10 days after a radio outburst, the radio source showed a constant flux density, which allowed sensitive imaging of the emission distribution. The structure in the map shows a clear extension to the southeast. Comparing our data with previous VLBI observations we interpret the extension as a collimated radio jet as found in several other X-ray binaries. Assuming that the structure is the result of an expansion that started at the onset of the outburst, we derive an apparent expansion velocity of 0.003 c, which, in the context of Doppler boosting, corresponds to an intrinsic velocity of at least 0.4 c for an ejection close to the line of sight. From the apparent velocity in all available epochs we are able to establish variations in the ejection angle which imply a precessing accretion disk. Finally we point out that LSI+61303, like SS433 and Cygnus X-1, shows evidence for an emission region almost orthogonal to the relativistic jet.

The extraordinarily bright optical afterglow of GRB 991208 and its host galaxy

Observations of the extraordinarily bright optical afterglow (OA) of GRB 991208 started 2.1 d after the event. The flux decay constant of the OA in the R-band is -2.30 +/- 0.07 up to 5 d, which is very likely due to the jet effect, and after that it is followed by a much steeper decay with constant -3.2 +/- 0.2, the fastest one ever seen in a GRB OA. A negative detection in several all-sky films taken simultaneously to the event implies either a previous additional break prior to 2 d after the occurrence of the GRB (as expected from the jet effect). The existence of a second break might indicate a steepening in the electron spectrum or the superposition of two events. Once the afterglow emission vanished, contribution of a bright underlying SN is found, but the light curve is not sufficiently well sampled to rule out a dust echo explanation. Our determination of z = 0.706 indicates that GRB 991208 is at 3.7 Gpc, implying an isotropic energy release of 1.15 x 10E53 erg which may be relaxed by beaming by a factor > 100. Precise astrometry indicates that the GRB coincides within 0.2' with the host galaxy, thus given support to a massive star origin. The absolute magnitude is M_B = -18.2, well below the knee of the galaxy luminosity function and we derive a star-forming rate of 11.5 +/- 7.1 Mo/yr. The quasi-simultaneous broad-band photometric spectral energy distribution of the afterglow is determined 3.5 day after the burst (Dec 12.0) implying a cooling frequency below the optical band, i.e. supporting a jet model with p = -2.30 as the index of the power-law electron distribution.

Optical nebulosities associated with IRAS sources in dense cloud cores

I, H¿ and [SII] CCD images of the regions around 4 young IRAS sources embedded in the dense molecular cloud cores CB 6, CB 39, AFGL 5142, and L 1251 are presented. Reflection nebulosities are found in all 4 regions. Herbig-Haro objects are detected in AFGL 5142 and L 1251. In both cases, the HH objects are new discoveries.

Two component Emden sphere

The theory of a self-gravitating gas sphere is given. The gravitational field is generated by two components, each of which is an independent isothermal gas. Various quantities of interest, such as density profiles, core radii of both components, masses, free-free luminosity, surface brightness, central surface density, and overestimate of central mass density, are given for different values of both parameters which arise naturally (ratio of central densities, ratio of rms velocities). Fundamental changes appear when comparison is made with a theory in which the second component is a 'test component'. Procedures are given for the complete analysis of real astrophysical configurations such as clusters of galaxies or globular clusters.

Faint arc-minute extended radio emission around Cygnus X-3

Aims.We revisit the vicinity of the microquasar Cygnus X-3 at radio wavelengths. We aim to improve our previous search for possible associated extended radio features/hot spots in the position angle of the Cygnus X-3 relativistic jets focusing on shorter angular scales than previously explored. Methods.Our work is mostly based on analyzing modern survey and archive radio data, mainly including observations carried out with the Very Large Array and the Ryle Telescopes. We also used deep near-infrared images that we obtained in 2005. Results.We present new radio maps of the Cygnus X-3 field computed after combining multi-configuration Very Large Array archive data at 6 cm and different observing runs at 2 cm with the Ryle Telescope. These are probably among the deepest radio images of Cygnus X-3 reported to date at cm wavelengths. Both interferometers reveal an extended radio feature within a few arc-minutes of the microquasar position, thus making our detection more credible. Moreover, this extended emission is possibly non-thermal, although this point still needs confirmation. Its physical connection with the microquasar is tentatively considered under different physical scenarios. We also report on the serendipitous discovery of a likely Fanaroff-Riley type II radio galaxy only away from Cygnus X-3.

Leptonic secondary emission in a hadronic microquasar model

Context.It has been proposed that the origin of the very high-energy photons emitted from high-mass X-ray binaries with jet-like features, so-called microquasars (MQs), is related to hadronic interactions between relativistic protons in the jet and cold protons of the stellar wind. Leptonic secondary emission should be calculated in a complete hadronic model that includes the effects of pairs from charged pion decays inside the jets and the emission from pairs generated by gamma-ray absorption in the photosphere of the system. Aims.We aim at predicting the broadband spectrum from a general hadronic microquasar model, taking into account the emission from secondaries created by charged pion decay inside the jet. Methods.The particle energy distribution for secondary leptons injected along the jets is consistently derived taking the energy losses into account. The spectral energy distribution resulting from these leptons is calculated after assuming different values of the magnetic field inside the jets. We also compute the spectrum of the gamma-rays produced by neutral pion-decay and processed by electromagnetic cascades under the stellar photon field. Results.We show that the secondary emission can dominate the spectral energy distribution at low energies (~1 MeV). At high energies, the production spectrum can be significantly distorted by the effect of electromagnetic cascades. These effects are phase-dependent, and some variability modulated by the orbital period is predicted.

Exploring the connection between the stellar wind and the non-thermal emission in LS 5039

Context.LS 5039 has been observed with several X-ray instruments so far showing quite steady emission in the long term and no signatures of accretion disk. The source also presents X-ray variability at orbital timescales in flux and photon index. The system harbors an O-type main sequence star with moderate mass-loss. At present, the link between the X-rays and the stellar wind is unclear. Aims.We study the X-ray fluxes, spectra, and absorption properties of LS 5039 at apastron and periastron passages during an epoch of enhanced stellar mass-loss, and the long term evolution of the latter in connection with the X-ray fluxes. Methods.New XMM-Newton observations were performed around periastron and apastron passages in September 2005, when the stellar wind activity was apparently higher. April 2005 Chandra observations on LS 5039 were revisited. Moreover, a compilation of H EW data obtained since 1992, from which the stellar mass-loss evolution can be approximately inferred, was carried out. Results.XMM-Newton observations show higher and harder emission around apastron than around periastron. No signatures of thermal emission or a reflection iron line indicating the presence of an accretion disk are found in the spectrum, and the hydrogen column density () is compatible with being the same in both observations and consistent with the interstellar value. 2005 Chandra observations show a hard X-ray spectrum, and possibly high fluxes, although pileup effects preclude conclusive results from being obtained. The H EW shows yearly variations of 10%, and does not seem to be correlated with X-ray fluxes obtained at similar phases, unlike what is expected in the wind accretion scenario. Conclusions.2005 XMM-Newton and Chandra observations are consistent with 2003 RXTE/PCA results, namely moderate flux and spectral variability at different orbital phases. The constancy of the seems to imply that either the X-ray emitter is located at 1012 cm from the compact object, or the density in the system is 3 to 27 times smaller than that predicted by a spherical symmetric wind model. We suggest that the multiwavelength non-thermal emission of LS 5039 is related to the observed extended radio jets and is unlikely to be produced inside the binary system.

Variable Very-High-Energy Gamma-Ray Emission from the Microquasar LS I +61 303

Microquasars are binary star systems with relativistic radio-emitting jets. They are potential sources of cosmic rays and can be used to elucidate the physics of relativistic jets. We report the detection of variable gamma-ray emission above 100 gigaelectron volts from the microquasar LS I 61 + 303. Six orbital cycles were recorded. Several detections occur at a similar orbital phase, which suggests that the emission is periodic. The strongest gamma-ray emission is not observed when the two stars are closest to one another, implying a strong orbital modulation of the emission or absorption processes.

Executive Summary, Feasibility Report on Proposed Amtrak Service Quad Cities-Chicago, January 7, 2008

Since the introduction of expanded levels of intrastate service on October 30, 2006, Amtrak trains in Illinois have produced impressive gains in both ridership and ticket revenue. This success and continuing stakeholder support has given rise to a formal request from the Illinois Department of Transportation (“Ill. DOT”) to Amtrak to develop a feasibility study regarding possible service consisting of a morning and an evening train in each direction between Chicago and the Quad Cities. The area between Chicago and the Quad Cities includes many rapidly growing communities. From Chicago toward the West and South, many towns and cities have experienced double digit growth increases in population since the year 2000. Southern DuPage, Cook and Will counties have seen especially strong growth, pressuring highway infrastructure, utilities, and schools. Community development and highway congestion are readily apparent when traveling the nearly 3 hour, 175 mile route between Chicago and the Quad Cities. As information, there are only three weekday round trip bus frequencies available between Chicago and the Quad Cities. The Quad City International Airport offers a total of 10 daily scheduled round trip flights to Chicago's O'Hare International Airport via two separate carriers flying regional jets. The Quad Cities (Davenport, Moline, Rock Island, and Bettendorf) are located along the Mississippi River. Nearly 60% of its visitors are from the Chicago area. With dozens of miles of scenic riverfront, river boating, casinos, and thousands of acres of expansive public spaces, the Quad Cities area is a major draw from both Iowa and Illinois. The huge Rock Island Arsenal, one of the largest military arsenals in the country and located along the river, is transitioning to become the headquarters of the United States First Army. As will be discussed later in the report, there is only one logical rail route through the Quad Cities themselves. The Iowa Interstate Railroad operates through the Quad Cities along the river and heads west through Iowa. The Quad Cities are considering at least three potential locations for an Amtrak station. A study now underway supported by several local stakeholders will recommend a site which will then be considered, given available local and other financial support. If Amtrak service were to terminate in the Quad Cities, an overnight storage track of sufficient length along with ample parking and certain other requirements covered elsewhere in the report would be required.

Iowa Rail Route Alternatives Analysis, June 1998

The development of new rail systems in the first part of the 21st century is the result of a wide range of trends that are making it increasingly difficult to maintain regional mobility using the two dominant intercity travel modes, auto and air. These trends include the changing character of the economic structure of industry. The character of the North American industrial structure is moving rapidly from a manufacturing base to a service based economy. This is increasing the need for business travel while the increase in disposable income due to higher salaries has promoted increased social and tourist travel. Another trend is the change in the regulatory environment. The trend towards deregulation has dramatically reduced the willingness of the airlines to operate from smaller airports and the level of service has fallen due to the creation of hub and spoke systems. While new air technology such as regional jets may mitigate this trend to some degree in medium-size airports, smaller airports will continue to lose out. Finally, increasing environmental concerns have reduced the ability of the automobile to meet intercity travel needs because of increased suburban congestion and limited highway capacity in big cities. Against this background the rail mode offers new options due to first, the existing rail rights-of-way offering direct access into major cities that, in most cases, have significant capacity available and, second, a revolution in vehicle technology that makes new rail rolling stock faster and less expensive to purchase and operate. This study is designed to evaluate the potential for rail service making an important contribution to maintaining regional mobility over the next 30 to 50 years in Iowa. The study evaluates the potential for rail service on three key routes across Iowa and assesses the impact of new train technology in reducing costs and improving rail service. The study also considers the potential for developing the system on an incremental basis. The service analysis and recommendations do not involve current Amtrak intercity service. That service is presumed to continue on its current route and schedule. The study builds from data and analyses that have been generated for the Midwest Rail Initiative (MWRI) Study. For example, the zone system and operating and capital unit cost assumptions are derived from the MWRI study. The MWRI represents a cooperative effort between nine Midwest states, Amtrak and the Federal Railroad Administration (FRA) contracting with Transportation Economics & Management Systems, Inc. to evaluate the potential for a regional rail system. The 1 The map represents the system including the decision on the Iowa route derived from the current study. Iowa Rail Route Alternatives Analysis TEMS 1-2 system is to offer modern, frequent, higher speed train service to the region, with Chicago as the connecting hub. Exhibit 1-1 illustrates the size of the system, and how the Iowa route fits in to the whole.

The 2010 May Flaring Episode of Cygnus X-3 in Radio, X-rays, and γ-rays

In 2009, Cygnus X-3 (Cyg X-3) became the first microquasar to be detected in the GeV γ-ray regime, via the satellites Fermi and AGILE. The addition of this new band to the observational toolbox holds promise for building a more detailed understanding of the relativistic jets of this and other systems. We present a rich data set of radio, hard and soft X-ray, and γ-ray observations of Cyg X-3 made during a flaring episode in 2010 May. We detect a ~3 day softening and recovery of the X-ray emission, followed almost immediately by a ~1 Jy radio flare at 15 GHz, followed by a 4.3σ γ-ray flare (E > 100 MeV) ~1.5 days later. The radio sampling is sparse, but we use archival data to argue that it is unlikely the γ-ray flare was followed by any significant unobserved radio flares. In this case, the sequencing of the observed events is difficult to explain in a model in which the γ-ray emission is due to inverse Compton scattering of the companion star's radiation field. Our observations suggest that other mechanisms may also be responsible for γ-ray emission from Cyg X-3.