Infrared Classification and Luminosities For Dusty AGN and the Most Luminous Quasars

Mid-infrared spectroscopic measurements from the Infrared Spectrometer on Spitzer (IRS) are given for 125 hard X-ray AGN (14-195 keV) from the Swift Burst Alert Telescope sample and for 32 AGN with black hole masses from reverberation mapping. The 9.7 um silicate feature in emission or absorption defines an infrared AGN classification describing whether AGN are observed through dust clouds, indicating that 55% of the BAT AGN are observed through dust. The mid-infrared dust continuum luminosity is shown to be an excellent indicator of intrinsic AGN luminosity, scaling closely with the hard X-ray luminosity, log vLv(7.8 um)/L(X) = -0.31 +- 0.35 and independent of classification determined from silicate emission or absorption. Dust luminosity scales closely with black hole mass, log vLv(7.8 um) = (37.2 +- 0.5) + 0.87 log BHM for luminosity in erg per sec and BHM in solar masses. The 100 most luminous type 1 quasars as measured in vLv(7.8 um) are found by comparing Sloan Digital Sky Survey optically discovered quasars with photometry at 22 um from the Wide-Field Infrared Survey Explorer, scaled to rest frame 7.8 um using an empirical template determined from IRS spectra. The most luminous SDSS/WISE quasars have the same maximum infrared luminosities for all 1.5 < z < 5, reaching total infrared luminosity L(IR) = 10^14.4 solar luminosities. Comparing with Dust Obscured Galaxies from Spitzer and WISE surveys, we find no evidence of hyperluminous obscured quasars whose maximum infrared luminosities exceed the maximum infrared luminosities of optically discovered quasars. Bolometric luminosities L(bol) estimated from rest frame optical or ultraviolet luminosities are compared to L(IR).Comment: accepted for publication in The Astrophysical Journa

Average Infrared Galaxy Spectra From Spitzer Flux Limited Samples

The mid-infrared spectroscopic analysis of a flux-limited sample of galaxies with fv(24um) > 10 mJy is presented. Sources observed are taken from the Spitzer First Look Survey (FLS) catalog and from the NOAO Deep Wide-Field Survey region in Bootes (NDWFS). The spectroscopic sample includes 60 of the 100 sources in these combined catalogs having fv(24um) > 10 mJy. New spectra from the Spitzer Infrared Spectrograph are presented for 25 FLS sources and for 11 Bootes AGN; these are combined with 24 Bootes starburst galaxies previously published to determine the distribution of mid-infrared spectral characteristics for the total 10 mJy sample. Sources have 0.01 < z < 2.4 and 41.8 < log vLv(15um) < 46.2 (ergs/s). Average spectra are determined as a function of luminosity; lower luminosity sources (log vLv(15um) < 44.0) are dominated by PAH features and higher luminosity sources (log vLv(15um) > 44.0) are dominated by silicate absorption or emission. We find that a rest frame equivalent width of 0.4um for the 6.2um PAH emission feature provides a well defined division between lower luminosity, "pure" starbursts and higher luminosity AGN or composite sources. Using the average spectra, fluxes fv(24um) which would be observed with the Spitzer MIPS are predicted as a function of redshift for sources with luminosities that correspond to the average spectra. AGN identical to those in this 10 mJy sample could be seen to z = 3 with fv(24um) > 1 mJy, but starbursts fall to fv(24um) < 1 mJy by z ~ 0.5. This indicates that substantial luminosity evolution of starbursts is required to explain the numerous starbursts found in other IRS results having fv(24um) > 1 mJy and z ~ 2.Comment: Accepted for publication in The Astrophysical Journa

The planning and construction of a double curved building in cross laminated timber (CLT) panels

This paper examines the planning and building process of a double curved building made of CNC cut cross laminated timber (CLT) panels. The paper explains the design of the shape, the construction process, and the choice of surface material. Still, the main focus is to investigate the practical experiences collected through the construction of such a non-tolerance-building set. The paper will look at what unforeseen challenges occurred on site during the construction. The main challenge for a building system consisting of perfect shaped panels, is that there is no room for adjustments during construction. Several characteristics of the shape of the building is belied to have caused trouble in terms of accuracy compared to a convex-only building with the same construction system. Another finding was that the engineer's choice of screws had an unexpected and significant impact on the construction process in terms of accuracy and construction time. For future development of the building system, there should be paid attention to means to either be able to build more accurately or there should be developed a way to adjust the position of the elements during the building process.acceptedVersio

Do Patients Judge Success of Treatment and Patient Acceptable Symptom State Based on Current Self-Reported Health Status?

Background: Value-based care models call for better interpretation of patient-reported outcomes. Patients may reference health status differently when appraising if an intervention was successful versus if their current state is acceptable. The purpose of this study was to determine the association between success of treatment (SOT), patient acceptable symptom state (PASS), and PROMIS measure T-scores, following a single primary care physical therapy encounter. Methods: Cross-sectional study. Ninety-two patients with musculoskeletal complaints were administered standard SOT and PASS questions, and PROMIS Physical Function, Pain Interference, and Self-Efficacy for Managing Symptoms measures. Association of PASS and SOT was determined using rank biserial correlation and chi-squared analysis. Accuracy of PROMIS T-scores to discriminate PASS and SOT was determined through receiver-operator curve analysis and likelihood ratios. Results: There was significant association between PASS and SOT (r=.393, p\u3c0.001; X2=15.7, p=0.001). The three PROMIS measures discriminated PASS with AUCs of 0.73 to 0.88 (accuracy 67.3% to 82.6%), Self-Efficacy being the strongest discriminator. Only Pain Interference T-scores discriminated SOT with AUC \u3e0.70 (accuracy 76.1%). Conclusion: PASS was more strongly associated with health status than SOT. Patients make a meaningful distinction between these two questions. Accurate clinician interpretation of PASS, SOT, and PROMIS T-scores can allow more targeted goal setting and treatment decision making

The Most Luminous Starbursts in the Universe

A summary of starburst luminosities based on PAH features is given for 243 starburst galaxies with 0 < z < 2.5, observed with the Spitzer Infrared Spectrograph. Luminosity vLv(7.7um) for the peak luminosity of the 7.7um PAH emission feature is found to scale as log[vLv(7.7um)] = 44.63(+-0.09) + 2.48(+-0.28)log(1+z) for the most luminous starbursts observed. Empirical calibrations of vLv(7.7um) are used to determine bolometric luminosity Lir and the star formation rate (SFR) for these starbursts. The most luminous starbursts found in this sample have log Lir = 45.4(+-0.3) + 2.5(+-0.3)log(1+z), in ergs per s, and the maximum star formation rates for starbursts in units of solar masses per yr are log(SFR) = 2.1(+-0.3) + 2.5(+-0.3)log(1+z), up to z = 2.5. The exponent for pure luminosity evolution agrees with optical and radio studies of starbursts but is flatter than previous results based in infrared source counts. The maximum star formation rates are similar to the maxima determined for submillimeter galaxies; the most luminous individual starburst included within the sample has log Lir = 46.9, which gives a SFR = 3400 solar masses per yr.Comment: Accepted for publication in The Astrophysical Journa

Infrared Spectra and Spectral Energy Distributions for Dusty Starbursts and AGN

We present spectroscopic results for all galaxies observed with the Spitzer Infrared Spectrograph (IRS) which also have total infrared fluxes f(ir) measured with the Infrared Astronomical Satellite (IRAS), also using AKARI photometry when available. Infrared luminosities and spectral energy distributions (SEDs) from 8 um to 160 um are compared to polycyclic aromatic hydrocarbon (PAH) emission from starburst galaxies or mid-infrared dust continuum from AGN at rest frame wavelengths ~ 8 um. A total of 301 spectra are analyzed for which IRS and IRAS include the same unresolved source, as measured by the ratio fv(IRAS 25 um)/fv(IRS 25 um). Sources have 0.004 < z < 0.34 and 42.5 < log L(IR) < 46.8 (erg per s) and cover the full range of starburst galaxy and AGN classifications. Individual spectra are provided electronically, but averages and dispersions are presented. We find that log [L(IR)/vLv(7.7 um)] = 0.74 +- 0.18 in starbursts, that log [L(IR)/vLv(7.7 um)] = 0.96 +- 0.26 in composite sources (starburst plus AGN), that log [L(IR)/vLv(7.9 um)] = 0.80 +- 0.25 in AGN with silicate absorption, and log [L(IR)/vLv(7.9 um)] = 0.51 +- 0.21 in AGN with silicate emission. L(IR) for the most luminous absorption and emission AGN are similar and 2.5 times larger than for the most luminous starbursts. AGN have systematically flatter SEDs than starbursts or composites, but their dispersion in SEDs overlaps starbursts. Sources with the strongest far-infrared luminosity from cool dust components are composite sources, indicating that these sources may contain the most obscured starbursts.Comment: Accepted for publication in The Astrophysical Journa

Evolving timber school building design in Norway

Due to the eminent importance of global sustainability, Norwegian municipalities as acting clients for school buildings, have initiated the usage of massive timber (Cross Laminated Timber) in new buildings. This paper is aiming to gain knowledge regarding the construction of massive timber school buildings by examining three case studies located in Norway. The findings suggest that appear to be four main factors that determine the choice and placement of material in the selected buildings: sustainability, topography, function and structure. Sustainability goals advocate maximization of usage of massive timber in the school buildings. Topography indicates that underground volumes are constructed in concrete and steel. Function and structure restrict the usage of CLT in main teaching spaces that have smaller spans, while acoustically challenging spaces like music rooms and auditoriums are constructed in steel and concrete. Literature also showed an evolution of massive timber construction in Norway, with contemporary architects and engineers achieving larger room spans than 10 years ago. Based on the findings, CLT construction is increasing and can change the way schools are being built in the Nordics.acceptedVersio

Evolution of the Most Luminous Dusty Galaxies

A summary of mid-infrared continuum luminosities arising from dust is given for very luminous galaxies, Lir > 10^12 solar luminosities, with 0.005 < z < 3.2 containing active galactic nuclei (AGN), including 115 obscured AGN and 60 unobscured (type 1) AGN. All sources have been observed with the Spitzer Infrared Spectrograph. Obscured AGN are defined as having optical depth > 0.7 in the 9.7 um silicate absorption feature and unobscured AGN show silicate in emission. Luminosity vLv(8 um) is found to scale as (1+z)^2.6 to z = 2.8, and luminosities vLv(8 um) are approximately 3 times greater for the most luminous unobscured AGN. Total infrared luminosities for the most luminous obscured AGN, Lir(AGN_obscured) in solar luminosities, scale as log Lir(AGN_obscured) = 12.3+-0.25 + 2.6(+-0.3)log(1+z), and for the most luminous unobscured AGN, scale as log Lir(AGN1) = 12.6+-0.15 + 2.6(+-0.3)log(1+z), indicating that the most luminous AGN are about 10 times more luminous than the most luminous starbursts. Results are consistent with obscured and unobscured AGN having the same total luminosities with differences arising only from orientation, such that the obscured AGN are observed through very dusty clouds which extinct about 50% of the intrinsic luminosity at 8 um. Both obscured and unobscured AGN should be detected to z ~ 6 by Spitzer surveys with fv(24 um) > 0.3 mJy, even without luminosity evolution for z > 2.5. By contrast, the most luminous starbursts cannot be detected for z > 3, even if luminosity evolution continues beyond z = 2.5.Comment: Includes corrected Figure 3, as publishe

Comparing Ultraviolet and Infrared-Selected Starburst Galaxies in Dust Obscuration and Luminosity

We present samples of starburst galaxies that represent the extremes discovered with infrared and ultraviolet observations, including 25 Markarian galaxies, 23 ultraviolet luminous galaxies discovered with GALEX, and the 50 starburst galaxies having the largest infrared/ultraviolet ratios. These sources have z < 0.5 and cover a luminosity range of ~ 10^4. Comparisons between infrared luminosities determined with the 7.7 um PAH feature and ultraviolet luminosities from the stellar continuum at 153 nm are used to determine obscuration in starbursts and dependence of this obscuration on infrared or ultraviolet luminosity. A strong selection effect arises for the ultraviolet-selected samples: the brightest sources appear bright because they have the least obscuration. Obscuration correction for the ultraviolet-selected Markarian+GALEX sample has the form log[UV(intrinsic)/UV(observed)] = 0.07(+-0.04)M(UV)+2.09+-0.69 but for the full infrared-selected Spitzer sample is log[UV(intrinsic)/UV(observed)] = 0.17(+-0.02)M(UV)+4.55+-0.4. The relation of total bolometric luminosity L_{ir} to M(UV) is also determined for infrared-selected and ultraviolet-selected samples. For ultraviolet-selected galaxies, log L_{ir} = -(0.33+-0.04)M(UV)+4.52+-0.69. For the full infrared-selected sample, log L_{ir} = -(0.23+-0.02)M(UV)+6.99+-0.41, all for L_{ir} in solar luminosities and M(UV) the AB magnitude at rest frame 153 nm. These results imply that obscuration corrections by factors of two to three determined from reddening of the ultraviolet continuum for Lyman Break Galaxies with z > 2 are insufficient, and should be at least a factor of 10 for M(UV) about -17, with decreasing correction for more luminous sources.Comment: accepted for publication in The Astrophysical Journa