DR9 Lyman-alpha forest sample

Introduction

One of the key science goals of BOSS was the measurement of the BAO
scale from the Lyman-alpha forest observed in the spectra of bright,
high redshift quasars. To aid in the analysis of the Lyman-alpha forest
from the first cosmological sample in BOSS, we selected objects suited
for Lyman-alpha forest studies and provide additional spectral products
to aid in the analysis.

The sample is described in detail in Lee et al. (2013). There are 3 main components to this sample:

Lists objects in our catalog, including information on SNR, fitted continuum, DLAs etc. Available in FITS and ASCII formats.
Individual spectra (speclya-[plate]-[mjd]-[fiberid].fits files)
Extension of the “lite” per-object spec files, with fluxes, pipeline errors, masks, correction vectors and continua. A Gzipped tarball is available for download here.
Flux artifact corrections
A global correction vector for the flux calibration artifacts noted by Busca et al. (2013) and Lee et al. (2013). Divide observed fluxes by this vector. Available as an ASCII file here.

Below we briefly summarize these products.

Sample Selection and Catalog

As a starting point, we use the BOSS DR9 Quasar Catalog (DR9Q). We make the following cuts on the catalog to select the objects suitable for Lyman-alpha forest analysis:

• z > 2.15 (using Z_VI visual inspection redshift from DR9Q)
• No BAL quasars (BAL_FLAG_VI=0 in DR9Q)
• S/N > 0.5 per pixel in 1268-1340 Å and S/N > 0.2 per pixel in 1041-1185 Å (restframe wavelengths)
• No more than 20% of pixels flagged by pipeline maskbit system
• Continua (see below) must be positive

The 54,468 selected objects are listed in a simple catalog, BOSSLyaDR9_cat, that is available in both FITS (4.3 MB) and ASCII (8.9 MB) formats. The detailed data model description of the catalog is available
here.

Individual Spectral Files

For each object in our catalog, we have generated an individual spectral file. These “speclya” files extend the “lite” per-object spec format with the following additional vectors in HDU 1:

Combined pixel mask system, incorporating pipeline masks (MASK_COMB = 1), a thorough sky emission line mask (MASK_COMB = 2), and masks for the central equivalent widths of Damped Lyman-alpha Absorbers (DLAs) detected by a combination of template-fitting (Noterdaeme et al. 2012) and Fisher Discriminant Analysis (Carithers et al., in prep) (MASK_COMB = 3). Pixels with MASK_COMB != 0 should be masked or discarded.
NOISE_CORR
A correction to ensure that the pipeline noise estimate is accurate to within several percent. This is derived by comparing the observed dispersion in the data with the pipeline estimate. The pipeline errors should be divided by this vector.
DLA_CORR
Corrections for damping wings of known DLAs in our spectra. While DLA cores are already masked by MASK_COMB, the damping wings suppresses the fluxes in the vicinity of the DLA. These corrections are derived using the absorption redshift Z_DLA and column-density LOG_NHI of the DLA, as listed in the BOSSLyaDR9_cat catalog. Multiply the observed fluxes by this vector to implement the correction.
CONT
Quasar continuum in the restframe 1040-1600 Ang region, estimated using a modified version of the MF-PCA method (Lee et al. 2012). Divide the observed fluxes by the continuum to extract the Lyman-alpha forest transmission.

All other HDUs in the spectra are unchanged from the “spec” files. The spectra in the DR9 Lyman-alpha Forest Sample can be downloaded in bulk here, where the individual spectra are grouped in sub-directories by plate number.

Flux Artifact Correction

There are 2-3% level artifacts, corresponding to observed Balmer wavelengths, in the average flux calibration of the DR9 spectra reduced by the v5_4_45 idlspec2d pipeline. These are caused by the interpolation over masked Balmer lines in the standard stars used to do flux calibration.

We derive a global correction for these artifacts by comparing continuum flux from ~29,000 quasars by their best-fit 1D pipeline model, available here. For a given spectrum, this correction vector should be interpolated to the given wavelength grid and used to divide the observed flux.

Usage Guidelines

To fully implement the DR9 Lyman-alpha Forest Sample, e.g., for comparing BAO measurements, all the objects in the BOSSDR9Lya_cat catalog should be used. For each spectrum (downloadable in bulk from here), the following operations should be performed:

  F = FLUX * DLA_CORR / (CONT * RESID)
SIGMA_F = (IVAR * RESID^2 * NOISE_CORR^2 * CONT^2 / DLA_CORR^2)^(-1/2)


where RESID is interpolated from residcorr_v5_4_45.dat . The Lyman-alpha forest interval is defined in 1041-1185 Å restframe with respect to Z_VI in BOSSLyaDR9_cat, and all pixels with MASK_COMB !=0 or IVAR=0 should be discarded or masked.