Far-infrared constraints on the contamination by dust-obscured galaxies of high-z dropout searches

The spectral energy distributions (SED) of dusty galaxies at intermediate redshift may look similar to very high-redshift galaxies in the optical/near infrared (NIR) domain. This can lead to the contamination of high-redshift galaxy searches based on broad-band optical/NIR photometry by lower redshift dusty galaxies because both kind of galaxies cannot be distinguished. The contamination rate could be as high as 50%. This work shows how the far-infrared (FIR) domain can help to recognize likely low-z interlopers in an optical/NIR search for high-z galaxies. We analyze the FIR SEDs of two galaxies that are proposed to be very high-redshift (z > 7) dropout candidates based on deep Hawk-I/VLT observations. The FIR SEDs are sampled with PACS/Herschel at 100 and 160 μm, with SPIRE/Herschel at 250, 350 and 500 μm and with LABOCA/APEX at 870 μm. We find that redshifts > 7 would imply extreme FIR SEDs (with dust temperatures >100 K and FIR luminosities >10^13 L_⊙). At z ~ 2, instead, the SEDs of both sources would be compatible with those of typical ultra luminous infrared galaxies or submillimeter galaxies. Considering all available data for these sources from visible to FIR we re-estimate the redshifts and find z ~ 1.6–2.5. Owing to the strong spectral breaks observed in these galaxies, standard templates from the literature fail to reproduce the visible-to-near-IR part of the SEDs even when additional extinction is included. These sources strongly resemble dust-obscured galaxies selected in Spitzer observations with extreme visible-to-FIR colors, and the galaxy GN10 at z = 4. Galaxies with similar SEDs could contaminate other high-redshift surveys.

Star formation in a stellar mass-selected sample of galaxies to z=3 from the GOODS-NICMOS Survey

We present a study of the star-forming properties of a stellar mass-selected sample of galaxies in the GOODS (Great Observatories Origins Deep Survey) NICMOS Survey (GNS), based on deep Hubble Space Telescope (HST) imaging of the GOODS North and South fields. Using a stellar mass-selected sample, combined with HST/ACS and Spitzer data to measure both ultraviolet (UV) and infrared-derived star formation rates (SFRs), we investigate the star forming properties of a complete sample of ∼1300 galaxies down to log M_*= 9.5 at redshifts 1.5 < z < 3. Eight per cent of the sample is made up of massive galaxies with M_*≥ 10^11 M_⊙. We derive optical colours, dust extinctions and UV and infrared SFR to determine how the SFR changes as a function of both stellar mass and time. Our results show that SFR increases at higher stellar mass such that massive galaxies nearly double their stellar mass from star formation alone over the redshift range studied, but the average value of SFR for a given stellar mass remains constant over this ∼2 Gyr period. Furthermore, we find no strong evolution in the SFR for our sample as a function of mass over our redshift range of interest; in particular we do not find a decline in the SFR among massive galaxies, as is seen at z < 1. The most massive galaxies in our sample (log M_*≥ 11) have high average SFRs with values SFR_UV, corr= 103 ± 75 M_⊙ yr^−1, and yet exhibit red rest-frame (U−B) colours at all redshifts. We conclude that the majority of these red high-redshift massive galaxies are red due to dust extinction. We find that A_2800 increases with stellar mass, and show that between 45 and 85 per cent of massive galaxies harbour dusty star formation. These results show that even just a few Gyr after the first galaxies appear, there are strong relations between the global physical properties of galaxies, driven by stellar mass or another underlying feature of galaxies strongly related to the stellar mass.

Local luminous infrared galaxies: Spatially resolved mid-infrared observations with Spitzer/IRS

Luminous Infrared (IR) Galaxies (LIRGs, L_IR=10^11-10 L_⨀) are an important cosmological class of galaxies as they are the main contributors to the co-moving star formation rate density of the universe at z=1. In this paper we present a guaranteed time observation (GTO) Spitzer InfraRed Spectrograph (IRS) program aimed to obtain spectral mapping of a sample of 14 local d<76Mpc LIRGs. The data cubes map, at least, the central 20arcsec X 20arcsec to 30 arcsec X 30 arcsec regions of the galaxies, and use all four IRS modules covering the full 5-38 μ m spectral range. The final goal of this project is to characterize fully the mid-IR properties of local LIRGs as a first step to understanding their more distant counterparts. In this paper we present the first results of this GTO program. The IRS spectral mapping data allow us to build spectral maps of the bright mid-IR emission lines (e.g., [Ne II] 12.81 μ m, [Ne III]15.56 μ m, [S III] 18.71 μ m, H_2 at 17 μ m), continuum, the 6.2 and 11.3 μ m polycyclic aromatic hydrocarbon (PAH) features, and the 9.7 μ m silicate feature, as well as to extract 1D spectra for regions of interest in each galaxy. The IRS data are used to obtain spatially resolved measurements of the extinction using the 9.7 μ m silicate feature, and to trace star forming regions using the neon lines and the PAH features. We also investigate a number of active galactic nuclei (AGN) indicators, including the presence of high excitation emission lines and a strong dust continuum emission at around 6 9.7 μ m . We finally use the integrated Spitzer/IRS spectra as templates of local LIRGs. We discuss several possible uses for these templates, including the calibration of the star formation rate of IR-bright galaxies at high redshift. We also predict the intensities of the brightest mid-IR emission lines for LIRGs as a function of redshift, and compare them with the expected sensitivities of future space IR missions.

The host galaxies and black holes of typical z~0.5-1.4 AGNs

We study the stellar and star formation properties of the host galaxies of 58 X-ray-selected AGNs in the GOODS portion of the Chandra Deep Field South (CDF-S) region at z ~ 0.5-1.4. The AGNs are selected such that their rest-frame UV to near-infrared spectral energy distributions (SEDs) are dominated by stellar emission; i.e., they show a prominent 1.6 μm bump, thus minimizing the AGN emission "contamination." This AGN population comprises approximately 50% of the X-ray-selected AGNs at these redshifts. We find that AGNs reside in the most massive galaxies at the redshifts probed here. Their characteristic stellar masses (M_* ~ 7.8 × 10^10 and M_* ~ 1.2 × 10^11 M_☉ at median redshifts of 0.67 and 1.07, respectively) appear to be representative of the X-ray-selected AGN population at these redshifts and are intermediate between those of local type 2 AGNs and high-redshift (z ~ 2) AGNs. The inferred black hole masses (M_BH ~ 2 × 10^8 M_☉) of typical AGNs are similar to those of optically identified quasars at similar redshifts. Since the AGNs in our sample are much less luminous (L_2–10 keV < 10^44 erg s^−1) than quasars, typical AGNs have low Eddington ratios (η ~ 0.01-0.001). This suggests that, at least at intermediate redshifts, the cosmic AGN "downsizing" is due to both a decrease in the characteristic stellar mass of typical host galaxies and less efficient accretion. Finally, there is no strong evidence in AGN host galaxies for either highly suppressed star formation (expected if AGNs played a role in quenching star formation) or elevated star formation when compared to mass-selected (i.e., IRAC-selected) galaxies of similar stellar masses and redshifts.

Spitzer power-law active galactic nucleus candidates in the chandra deep field-north

We define a sample of 62 galaxies in the Chandra Deep Field-North whose Spitzer IRAC SEDs exhibit the characteristic power-law emission expected of luminous AGNs. We study the multiwavelength properties of this sample and compare the AGNs selected in this way to those selected via other Spitzer color-color criteria. Only 55% of the power-law galaxies are detected in the X-ray catalog at exposures of >0.5 Ms, although a search for faint emission results in the detection of 85% of the power-law galaxies at the ≥2.5 σ detection level. Most of the remaining galaxies are likely to host AGNs that are heavily obscured in the X-ray. Because the power-law selection requires the AGNs to be energetically dominant in the near- and mid-infrared, the power-law galaxies comprise a significant fraction of the Spitzer-detected AGN population at high luminosities and redshifts. The high 24 μm detection fraction also points to a luminous population. The power-law galaxies comprise a subset of color-selected AGN candidates. A comparison with various mid-infrared color selection criteria demonstrates that while the color-selected samples contain a larger fraction of the X-ray-luminous AGNs, there is evidence that these selection techniques also suffer from a higher degree of contamination by star-forming galaxies in the deepest exposures. Considering only those power-law galaxies detected in the X-ray catalog, we derive an obscured fraction of 68% (2 : 1). Including all of the power-law galaxies suggests an obscured fraction of <81% (4 : 1).

Near-infrared and star-forming properties of local luminous infrared galaxies

We use Hubble Space Telescope (HST) NICMOS continuum and Paα observations to study the near-infrared and star formation properties of a representative sample of 30 local (d ~ 35-75 Mpc) luminous infrared galaxies (LIRGs, infrared [8-1000 μm] luminosities of log L_IR = 11-11.9 L_☉). The data provide spatial resolutions of 25-50 pc and cover the central ~3.3-7.1 kpc regions of these galaxies. About half of the LIRGs show compact (~1-2 kpc) Paα emission with a high surface brightness in the form of nuclear emission, rings, and minispirals. The rest of the sample show Paα emission along the disk and the spiral arms extending over scales of 3-7 kpc and larger. About half of the sample contains H II regions with Hα luminosities significantly higher than those observed in normal galaxies. There is a linear empirical relationship between the mid-IR 24 μm and hydrogen recombination (extinction-corrected Paα) luminosity for these LIRGs, and the H II regions in the central part of M51. This relation holds over more than four decades in luminosity, suggesting that the mid-IR emission is a good tracer of the star formation rate (SFR). Analogous to the widely used relation between the SFR and total IR luminosity of R. Kennicutt, we derive an empirical calibration of the SFR in terms of the monochromatic 24 μm luminosity that can be used for luminous, dusty galaxies.

Evaluating the Sandcastles Program: A Group Intervention for Children of Divorce

The Sandcastles program has been utilized nationwide as a one-time group intervention to assist children of divorcing parents. For several years Miami-Dade family court services mandated participation in the program for divorcing or separating families. Currently, there is a paucity of research and evaluation to ascertain the efficacy of the program. This symposium will provide details and discussion regarding the planning and process used to establish an evaluation plan to assess the effectiveness of the Sandcastles program for families in MiamiDade County. Any preliminary outcomes available at the time of the symposium will also be shared.

(Table 1, page 126) Concentration of elements in Fe and Mn rich pisoliths (nodules) from Lake Storsjoen, South Norway

A detailed description of the ores of Lake Storsjoen was given by Vogt J. H. L., 1915 who pointed out that the ores may be divided into two principal types; first, iron ore with 2% or less of manganese (ex: Ertemalm), and, second, ores with manganese contents of up to 30% (ex: Korinter). The iron-rich ore sometimes occurs as a conglomerate embedded in manganese-rich ores, clearly demonstrating that two distinctly different precipitates are involved. In the iron-rich ore, a concentric structure is common of which light brown layers of loose, almost dusty material alternate with hard and brittle black layers, the thickness of each being 0.5 mm or less. The analyses presented in this paper seem to demonstrate that the composition of the sedimentary ores of Lake Storsjden could result from fluctuations in the composition of ground waters feeding the lake.

(Table 2) Seasonal flux data and percentages of major bulk components of total flux at the mesotrophic sediment trap site CB from 1988 - 2012

A more than two-decadal sediment trap record from the Eastern Boundary Upwelling Ecosystem (EBUE) off Cape Blanc, Mauritania, is analysed with respect to deep ocean mass fluxes, flux components and their variability on seasonal to decadal timescales. The total mass flux revealed interannual fluctuations which were superimposed by fluctuations on decadal timescales. High winter fluxes of biogenic silica (BSi), used as a measure of marine production (mostly by diatoms) largely correspond to a positive North Atlantic Oscillation (NAO) index (December-March). However, this relationship is weak. The highest positive BSi anomaly was in winter 2004-2005 when the NAO was in a neutral state. More episodic BSi sedimentation events occurred in several summer seasons between 2001 and 2005, when the previous winter NAO was neutral or even negative. We suggest that distinct dust outbreaks and deposition in the surface ocean in winter and occasionally in summer/autumn enhanced particle sedimentation and carbon export on short timescales via the ballasting effect. Episodic perturbations of the marine carbon cycle by dust outbreaks (e.g. in 2005) might have weakened the relationships between fluxes and large-scale climatic oscillations. As phytoplankton biomass is high throughout the year, any dry (in winter) or wet (in summer) deposition of fine-grained dust particles is assumed to enhance the efficiency of the biological pump by incorporating dust into dense and fast settling organic-rich aggregates. A good correspondence between BSi and dust fluxes was observed for the dusty year 2005, following a period of rather dry conditions in the Sahara/Sahel region. Large changes of all bulk fluxes occurred during the strongest El Niño-Southern Oscillation (ENSO) in 1997-1999 where low fluxes were obtained for almost 1 year during the warm El Niño and high fluxes in the following cold La Niña phase. For decadal timescales, Bakun (1990) suggested an intensification of coastal upwelling due to increased winds (''Bakun upwelling intensification hypothesis''; Cropper et al., 2014) and global climate change. We did not observe an increase of any flux component off Cape Blanc during the past 2 and a half decades which might support this. Furthermore, fluxes of mineral dust did not show any positive or negative trends over time which might suggest enhanced desertification or ''Saharan greening'' during the last few decades.

Diálogo con Europa, diálogo con el pasado. Antepasados y tradición entre la nobleza colonial nahua

En este trabajo presentamos un acercamiento a los modos de referirse al pasado en los testimonios dejados por los miembros de la nobleza colonial nahua. La lectura de las fuentes nos permite distinguir dos perspectivas –intelectual y pragmática– asociadas respectivamente con el proyecto de unir las tradiciones históricas indígena y europea y con la búsqueda de argumentos en la lucha por tierras y privilegios. El enfoque del artículo son los conceptos nahuas de «tradición» y «antepasados» (huehuetqueh), manifiestos en ambas perspectivas. Al analizar el vocabulario, retórica e iconografía intentamos entender el significado de estos conceptos dentro de la cultura nahua prehispánica y su modificación bajo las circunstancias coloniales, tanto como su papel en la continuación de la identidad nahua.

Relaciones interétnicas en el Fuerte San José (Patagonia, siglo XVIII). Una aproximación comparativa

El presente trabajo tiene por objeto presentar la primera aproximación a las relaciones interétnicas en el escenario del Fuerte San José y el Puesto de la Fuente, desde una perspectiva histórica y arqueológica. En particular, presentaremos los primeros resultados de las investigaciones históricas respecto de la problemática mencionada, sobre la base de información inédita analizada hasta el momento. Para ello nos centraremos en los primeros diez años de vida en el Fuerte (1779-1789) y estableceremos una comparación con los otros dos asentamientos que formaron parte del plan de poblamiento español de las costa patagónica (siglo XVIII): el Fuerte Nuestra Señora del Carmen y la Nueva Colonia de Floridablanca, a los efectos de destacar la particularidad del Fuerte San José en el marco de la variabilidad de la estructuración de las relaciones interétnicas en las colonias patagónicas.

Entre reglas y excepciones. Es decir, como legitimar las decisiones colectivas

El ensayo examina la cuestión de la aplicación de las reglas y de la capacidad real para tratar casos específicos, llegando a la conclusión de que es la excepción la que confirma la regla, a condición de que sea dialógicamente construida, para que sea interpretable y aplicable por parte de sus numerosos destinatarios en las políticas públicas más complejas y conflictuales, sobre todo a nivel local.

Testing quasar unification: radiative transfer in clumpy winds

Various unification schemes interpret the complex phenomenology of quasars and luminous active galactic nuclei (AGN) in terms of a simple picture involving a central black hole, an accretion disc and an associated outflow. Here, we continue our tests of this paradigm by comparing quasar spectra to synthetic spectra of biconical disc wind models, produced with our state-of-the-art Monte Carlo radiative transfer code. Previously, we have shown that we could produce synthetic spectra resembling those of observed broad absorption line (BAL) quasars, but only if the X-ray luminosity was limited to 1043 erg s-1. Here, we introduce a simple treatment of clumping, and find that a filling factor of ˜0.01 moderates the ionization state sufficiently for BAL features to form in the rest-frame UV at more realistic X-ray luminosities. Our fiducial model shows good agreement with AGN X-ray properties and the wind produces strong line emission in, e.g., Lyα and C IV 1550 Å at low inclinations. At high inclinations, the spectra possess prominent LoBAL features. Despite these successes, we cannot reproduce all emission lines seen in quasar spectra with the correct equivalent-width ratios, and we find an angular dependence of emission line equivalent width despite the similarities in the observed emission line properties of BAL and non-BAL quasars. Overall, our work suggests that biconical winds can reproduce much of the qualitative behaviour expected from a unified model, but we cannot yet provide quantitative matches with quasar properties at all viewing angles. Whether disc winds can successfully unify quasars is therefore still an open question.

Nuclei of Nearby Active Galaxies: NIR and Sub-mm Views and Finalizing the LINC-NIRVANA Fringe and Flexure Tracking System: Flexure and Temperature Behavior

The work presented in my thesis addresses the two cornerstones of modern astronomy: Observation and Instrumentation. Part I deals with the observation of two nearby active galaxies, the Seyfert 2 galaxy NGC 1433 and the Seyfert 1 galaxy NGC 1566, both at a distance of $\sim10$ Mpc, which are part of the Nuclei of Galaxies (NUGA) sample. It is well established that every galaxy harbors a super massive black hole (SMBH) at its center. Furthermore, there seems to be a fundamental correlation between the stellar bulge and SMBH masses. Simulations show that massive feedback, e.g., powerful outflows, in Quasi Stellar Objects (QSOs) has an impact on the mutual growth of bulge and SMBH. Nearby galaxies follow this relation but accrete mass at much lower rates. This gives rise to the following questions: Which mechanisms allow feeding of nearby Active Galactic Nuclei (AGN)? Is this feeding triggered by events, e.g., star formation, nuclear spirals, outflows, on $\sim500$ pc scales around the AGN? Does feedback on these scales play a role in quenching the feeding process? Does it have an effect on the star formation close to the nucleus? To answer these questions I have carried out observations with the Spectrograph for INtegral Field Observation in the Near Infrared (SINFONI) at the Very Large Telescope (VLT) situated on Cerro Paranal in Chile. I have reduced and analyzed the recorded data, which contain spatial and spectral information in the H-band ($1.45 \mic-1.85 \mic$) and K-band ($1.95 \mic-2.45 \mic$) on the central $10\arcsec\times10\arcsec$ of the observed galaxies. Additionally, Atacama Large Millimeter/Sub-millimeter Array (ALMA) data at $350$ GHz ($\sim0.87$ mm) as well as optical high resolution Hubble Space Telescope (HST) images are used for the analysis. For NGC 1433 I deduce from comparison of the distributions of gas, dust, and intensity of highly ionized emission lines that the galaxy center lies $\sim70$ pc north-northwest of the prior estimate. A velocity gradient is observed at the new center, which I interpret as a bipolar outflow, a circum nuclear disk, or a combination of both. At least one dust and gas arm leads from a $r\sim200$ pc ring towards the nucleus and might feed the SMBH. Two bright warm H$_2$ gas spots are detected that indicate hidden star formation or a spiral arm-arm interaction. From the stellar velocity dispersion (SVD) I estimate a SMBH mass of $\sim1.74\times10^7$ \msol. For NGC 1566 I observe a nuclear gas disk of $\sim150$ pc in radius with a spiral structure. I estimate the total mass of this disk to be $\sim5.4\times10^7$ \msol. What mechanisms excite the gas in the disk is not clear. Neither can the existence of outflows be proven nor is star formation detected over the whole disk. On one side of the spiral structure I detect a star forming region with an estimated star formation rate of $\sim2.6\times10^{-3}$ \msol\ yr$^{-1}$. From broad Br$\gamma$ emission and SVD I estimate a mean SMBH mass of $\sim5.3\times10^6$ \msol\ with an Eddington ratio of $\sim2\times10^{-3}$. Part II deals with the final tests of the Fringe and Flexure Tracker (FFTS) for LBT INterferometric Camera and the NIR/Visible Adaptive iNterferometer for Astronomy (LINC-NIRVANA) at the Large Binocular Telescope (LBT) in Arizona, USA, which I conducted. The FFTS is the subsystem that combines the two separate beams of the LBT and enables near-infrared interferometry with a significantly large field of view. The FFTS has a cryogenic system and an ambient temperature system which are separated by the baffle system. I redesigned this baffle to guarantee the functionality of the system after the final tests in the Cologne cryostat. The redesign did not affect any scientific performance of LINC-NIRVANA. I show in the final cooldown tests that the baffle fulfills the temperature requirement and stays $<110$ K whereas the moving stages in the ambient system stay $>273$ K, which was not given for the old baffle design. Additionally, I test the tilting flexure of the whole FFTS and show that accurate positioning of the detector and the tracking during observation can be guaranteed.

Pyhäjoen Vanhatien toimenpidesuunnitelma

Pyhäjoen asukasmäärän ennustetaan kasvavan ydinvoimalan rakentamisen myötä. Kasvu näkyy myös taajamassa, missä sekä yleis- että asemakaava mahdollistavat uusien asuinalueiden rakentamisen ja keskusta-alueen tiivistämisen ja laajentamisen. Suunnittelukohteena on Pyhäjoen Vanhatie ja Virastotie, jotka ovat taajaman sisäisen liikenteen tärkeimmät väylät. Suunnittelu tehdään ydinkeskustan alueella seinästä seinään. Suunnittelukohteena on myös valtatien liittymät sekä tori. Suunnittelualueen liikennemäärät ovat vähäisiä, eikä liikenteellisiä ongelmia ennusteta syntyvän, vaikka liikennemäärä kasvaisikin suhteellisesti paljon. Eniten liikennettä on taajaman sivuitse menevällä valtatiellä 8 ja sen liittymissä liikenteen lisäys näkynee onnettomuuksien kasvuna, jos mitään toimenpiteitä ei tehtäisi. Tiet ovat rakenteelltaan kohtuullisessa kunnossa, joskin kuluneita. Ympäristöllisesti suunnittelualue on mielenkiintoinen, sillä Vanhatie on osa Pohjanlahden Rantatietä ja sillä onkin matkailutie-status. Tie on raittimainen, ja sen varrella on useita mielenkiintoisia kohteita, kuten vanhat rakennukset ja puut sekä kalliopaljastumat. Suunnittelujakson eteläpäässä on Etelänkylän Isosilta, joka on Suomen vanhin liikennekäytössä oleva puusilta. Se onkin museosilta. Silta on huonokuntoinen. Tavoitteena on löytää toteuttamiskelpoiset toimenpiteet, joilla ydinkeskusta-alueella tien luonnetta muutetaan keskustamaisemmaksi kaduksi. Torin ja ydinkeskustan yleisilme on tehtävä nykyistä houkuttelevammaksi myös ohikulkevien silmissä. Tavoitteena on saada valtatien kulkijat pistäytymään Pyhäjoella. Kyseiset väylät ovat toistaiseksi maanteitä, mutta tavoitteena on toimenpiteiden toteuttamisen jälkeen muuttaa ne kaduiksi. Toimenpide-esitykset ovat keskittyneet ydinkeskustan alueelle. Vanhatien ja Virastotien liittymäalue sekä kunnantalon edusta rakennetaan torimaiseksi aukioksi. Alue muuttuu yhteistilaksi, jossa jalankulku ja pyöräily on helppoa ja turvallista. Tapahtumia on helppo tarvittaessa laajentaa liikennenalueille. Samoja periaatteita käytetään torin parantamisessa, jossa tori laajenee visuaalisesti Vanhatielle. Suunnittelu on tehty siitä lähtökohdasta, että tori säilyy nykypaikallaan ja mahdollinen Pyhäjoki-talo rakennetaan nykyisen Salen paikalla torin pariksi. Valtatieliittymistä Virastotien liittymän parantaminen on jo suunniteltu aiemmin. Tiiranmaantien liittymä esitetään porrastettavaksi yleiskaavan periaatteen mukaisesti. Vihannintien liittymään rakennetaan turvasaarekket. Merkittävä toimenpide on esitys erityiskohteiden valaisemiseksi. Niitä ovat muun muassa sillat, vanhat isot puut, kalliopaljastumat ja osin myös vanhat rakennuksetkin. Muualla toimenpiteet ovat lähinnä jalankulku- ja pyöräteiden täydentämistä ja viheralueiden kunnostamista. Esitetyt toimenpiteet mahdollistavat kaavojen toteuttamisen. Muutamassa kohdassa asemakaavaa on muutetava toimenpiteiden mahdollistamiseksi. Lähiympäristö paranee, kun katupuita uusitaan ja täydennetään. Rakentamisen kustannukset ovat yhteensä noin 5,2 miljoonaa euroa (alv 0%).