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A photometric UBV survey is presented for 610 stars in a region surroundingthe Cepheid AQ Puppis and centered southwest of the variable, based uponphotoelectric measures for 14 stars and calibrated iris photometry ofphotographic plates of the field for 596 stars. An analysis of reddening anddistance for program stars indicates that the major dust complex in thisdirection is ~1.8 kpc distant, producing differential extinction described by aratio of total-to-selective extinction of R=Av/E(B-V)=3.10+-0.20. Zero-agemain-sequence fitting for the main group of B-type stars along the line ofsight yields a distance of 3.21+-0.19 kpc (Vo-Mv=12.53+-0.13 s.e.). The 29.97dCepheid AQ Pup, of field reddening E(B-V)=0.47+-0.07 (E(B-V)(B0)=0.51+-0.07),appears to be associated with B-type stars lying within 5' of it as well aswith a sparse group of stars, designated Turner 14, centered south of it atJ2000.0 = 07:58:37, -29:25:00, with a mean reddening of E(B-V)=0.81+-0.01. AQPup has an inferred luminosity as a cluster member of <Mv>=-5.40+-0.25 and anevolutionary age of 3x10^7 yr. Its observed rate of period increase of300.1+-1.2 s/yr is an order of magnitude larger than what is observed forCepheids of comparable period in the third crossing of the instability strip,and may be indicative of a high rate of mass loss or a putative fifth crossing.Another sparse cluster, designated Turner 13, surrounds the newly-recognized2.59d Cepheid V620 Pup, of space reddening E(B-V)=0.64+-0.02(E(B-V)(B0)=0.68+-0.02), distance 2.88+-0.11 kpc (Vo-Mv=12.30+-0.08 s.e.),evolutionary age 10^8 yr, and an inferred luminosity as a likely cluster memberof <Mv>=-2.74+-0.11. V620 Pup is tentatively identified as a first crosser,pending additional observations.

A Search for OB Associations Near Southern Long-Period Cepheids. V. AQ Puppis and V620 Puppis